1005 I/5 Proper Motions in Cape Zone Catalogue -40/-52 J H Spencer J Jackson His Majesty's Stationery Office, London ??? ??? 1936 Positional data Proper motions This catalog, listing the proper motions of 20,843 stars from the Cape Astrographic Zones, was compiled from three series of photographic plates. The plates were taken at the Royal Observatory, Cape of Good Hope, in the following years: 1892-1896, 1897-1910, 1923-1928. Data given include centennial proper motion, photographic and visual magnitude, Harvard spectral type, Cape Photographic Durchmusterung (CPD) identification, epoch, right ascension and declination for 1900.

--- Number 5 --- CZC Catalogue Identification Number --- Vmag Visual Magnitude mag RAh Right Ascension for 1900 hours h RAm Right Ascension for 1900 minutes min RAcs Right Ascension seconds in 0.01sec 1900 0.01s DE- Declination Sign --- DEd Declination for 1900 degrees deg DEm Declination for 1900 arcminutes arcmin DEds Declination for 1900 arcseconds 0.1arcsec Ep-1900 Epoch -1900 cyr CPDZone Cape Photographic Durchmusterung Zone --- CPDNo Cape Photographic Durchmusterung Number --- Pmag Photographic Magnitude mag Sp HD Spectral Type --- pmRAs Proper Motion in RA the relation is pmRA = 15 * pmRAs * cos(DE) if pmRAs is expressed in s/yr and pmRA in arcsec/yr 0.1ms/yr pmRA Proper Motion in RA mas/yr pmDE Proper Motion in Dec mas/yr Julie Anne Watko SSDOO/ADC 1995 Nov 03 I_5.xml 1006 I/6 Cape 20554 Faint Stars, -40 to -52, 1900.0 J H Spencer J Jackson His Majesty's Stationery Office, London ??? ??? 1939 1939HMSO..C......0S Positional data Proper motions This catalog contains positions, precessions, proper motions, and photographic magnitudes for 20,554 stars. These were derived from photographs taken at the Royal Observatory, Cape of Good Hope between 1923 and 1928. It covers the astrographic zones -40 degrees to -52 degrees of declination. The positions are given for epoch 1900 (1900.0). It includes spectral types for many of the stars listed. It extends the earlier catalogs derived from the same plates to fainter magnitudes. The computer-readable version consists of a single data table. The stated probable error for the star positions is 0.024 seconds of time (R.A.) and 0.25 seconds of arc (dec.) for stars with one determination, 0.017 seconds of time, and 0.18 seconds of arc for two determinations, and 0.014 / 0.15 for stars with three determinations. The precession and secular variations were derived from Newcomb's constants. The authors quote probable errors of the proper motions in both coordinates of 0.008 seconds of arc for stars with one determination, 0.0055 seconds for stars with two determinations, and 0.0044 for stars with three. The photographic magnitudes were derived from the measured diameters on the photographic plates and from the magnitudes given in the Cape Photographic Durchmusterung. The spectral classification of the cataloged stars was done with the assistance of Annie Jump Cannon of the Harvard College Observatory. The user should consult the source reference for more details of the measurements and reductions. See also the notes in this document for additional information on the interpretation of the entries.

ID Cape Number --- rem Remark A = Astrographic Star F = Faint Proper Motion Star N = Other Note --- CPDZone Cape Phot. Durchmusterung (CPD) Zone All CPD Zones are negative. - signs are not included in data. "0" in column 8 signifies Astrographic Plate instead of CPD. --- CPD CPD Number or Astrographic Plate See also note on CPDZone. Astrographic plate listed "is the more southerly on which the star occurs." Thus, y-coordinate is positive wherever possible. --- n_CPD [1234] Remarks A number from 1-4 appears in this byte for double stars where the same CPD number applies to more than one star. --- mpg Photographic Magnitude The Photographic Magnitude is "determined from the CPD Magnitude and the diameter on the Cape Astrographic Plates by means of the data given in the volume on the Magnitudes of Stars in the Cape Zone Catalogue." A null value (99.9) signifies a variable star. mag RAh Mean Right Ascension hours 1900 h RAm Mean Right Ascension minutes 1900 min RAs Mean Right Ascension seconds 1900 s DEd Mean Declination degrees 1900 deg DEm Mean Declination arcminutes 1900 arcmin DEs Mean Declination arcseconds 1900 arcsec N Number of Observations --- Epoch Epoch +1900 yr pmRA Proper Motion in RA seconds of time s/a pmRAas Proper Motion in RA arcseconds arcsec/a pmDE Proper Motion in Dec arcseconds arcsec/a Sp HD Spectral Type --- Julie Anne Watko SSDOO/ADC 1996 Mar 26 I_6.xml 1014 I/14 Proper Motions of 1160 Late-Type Stars H J Fogh Olsen Astron. Astrophys. Suppl. Ser. 2 69 1970 1970A&AS....2...69O II/38 : Stars observed photoelectrically by Dickow et al. Fogh Olsen H.J. 1970, Astron. Astrophys. Suppl. Ser., 2, 69. Fogh Olsen H.J. 1970, Astron. Astrophys., Suppl. Ser., 1, 189. Proper motions Improved proper motions for the 1160 stars contained in the photometric catalog by Dickow et al. (1970) are presented. Most of the proper motions are from the GC, transferred to the system of FK4. For stars not included in the GC, preliminary AGK or SAO proper motions are given. Fogh Olsen (Astron. Astrophys. Suppl. Ser., 1, 189, 1970) describes the method of improvement. The mean errors of the centennial proper motions increase with increasing magnitude. In Right Ascension, these range from 0.0043/cos(dec) for very bright stars to 0.096/cos(dec) for the faintest stars. In Dec- lination, the range is from 0.065 to 1.14.

No Number Henry Draper or Bonner Durchmusterung number --- pmRA Centennial Proper Motion RA s/ca pmDE Centennial Proper Motion Dec arcsec/ca RV Radial Velocity km/s Julie Anne Watko ADC 1996 Jun 03 I_14.xml 1016 I/16 Catalog of 3356 Faint Stars, 1950 J Larink A Bohrmann H Kox J Groeneveld H Klauder Verlag der Sternwarte, Hamburg-Bergedorf ??? ??? 1955 1955 Fundamental catalog Positional data Proper motions This catalog of 3356 faint stars was derived from meridian circle observations at the Bergedorf and Heidelberg Observatories. The positions are given for the equinox 1950 on the FK3 system. The stars are mainly between 8.0 and 10.0 visual magnitude. A few are brighter than 8.0 mag. The lower limit in brightness resulted from the visibility of the stars.

All stars were observed at both the Heidelberg and Bergedorf Observatories. Normally, at each observatory, two observations were obtained with the clamp east and two with the clamp west. The mean errors are comparable for the two observatories with no significant systematic difference in the positions between them. The mean errors of the resulting positions should be approximated 0.011s/cos(dec) in right ascension and ).023" in declination. The proper motions were derived from a comparison with the catalog positions with the positions in the AGK2 and AGK2A with a 19 year baseline and from a comparison of new positions with those in Kuestner 1900 with about a fifty year baseline. The magnitudes were taken from the AGK2. Most spectral types were determined by A. N. Vyssotsky. A few are from the Bergedorfer Spektraldurchmusterung.

ID Catalog number --- DMz BD zone --- DMn BD number --- mag Photographic magnitude mag Sp Spectral class --- RAh Right Ascension hours (1950) h RAm Right Ascension minutes (1950) min RAs Right Ascension seconds (1950) s Pr-RA1 First order precession in RA per century 0.01s/a Pr-RA2 Second order precession in RA per century 0.0001s2/a2 pmRA Proper motion in RA from AGK2 positions 0.01s/a pmRA2 Proper motion in RA from Kuestner positions 0.01s/a DE- Sign of declination (1950) --- DEd Declination degrees (1950) deg DEm Declination minutes (1950) arcmin DEs Declination seconds (1950) arcsec Pr-de1 First order precession in dec per century arcsec/ha Pr-de2 Second order precession in dec per century arcsec2/ha2 pmdec Proper motion in DE from AGK2 positions arcsec/ha pmdec2 Proper motion in DE from Kuestner positions arcsec/ha epoch Epoch of observation - 1900.0 yr rem Note for star in printed catalog 1 = ma (blend?) 3 = pr (preceding) 4 = seq (following) 5 = bor (northern) 6 = au (southern) * = other note in printed volume (All notes in the printed volume have not been indicated in this version.) the printed volume sometimes has additional information on the systems with numerical remarks. --- Nancy Grace Roman ADC/SSDOO 1996 Feb 01 I_16.xml 1021A I/21A AC Toulouse, Bordeaux, Paris & Oxford P Lacroute A Valbousquet CDS Bull. No. 6, p. 38 ??? ??? 1974 1974BICDS...6...38L Astrographic zones Magnitudes, photographic Positional data The "Carte de Ciel" (or "Astrographic Catalogue") is a catalogue of star positions and magnitudes, determined on the photographic plates taken by the normal astrographs which are installed in observatories of various latitudes, as a world-wide astronomical project (see Eichhorn, 1974, p279). The catalogue is divided into 22 declination zones, each of which is assigned to each observatory, e.g., a zone from +18 to +24 degrees is to Paris observatory. Each observatory has taken photographs of 2 deg x 2 deg area in and covering each zone, measured the X,Y coordinates of star images on the photographic plates, and published the results as the printed catalogues. The present catalogue is the results of reduction of these X,Y coordinates into right ascension and declination values, for declination zones of +05 to +31, by using AGK2/3 catalogue as the reference.

ZONE plate identifier declination zone, or the declination of the center of each astrographic plate deg PLATE plate identifier running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. --- HYPH hyphen number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- STAR running number of star on the plate number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- RAh right ascension (hours) [B1950] number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. h RAm right ascension (minutes) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. min RAs ascension (seconds) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. s DE- declination sign number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- DEd declination (degrees) [B1950] number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. deg DEm declination (minutes) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. arcmin DEs declination (seconds) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. arcsec EPOCH plate epoch number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. a mB photographic magnitude number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. mag AGKNO AGK2 number AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- SUFFIX suffix to the AGK2 number Suffix to the AGK2 number, if needed, otherwise CR/LF. number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- ZONE plate identifier declination zone, or the declination of the center of each astrographic plate deg PLATE plate identifier running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. --- HYPH hyphen number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- STAR running number of star on the plate number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- RAh right ascension (hours) [B1950] number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. h RAm right ascension (minutes) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. min RAs ascension (seconds) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. s DE- declination sign number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- DEd declination (degrees) [B1950] number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. deg DEm declination (minutes) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. arcmin DEs declination (seconds) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. arcsec EPOCH plate epoch number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. a mB photographic magnitude number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. mag AGKNO AGK2 number AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- SUFFIX suffix to the AGK2 number Suffix to the AGK2 number, if needed, otherwise CR/LF. number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- ZONE plate identifier declination zone, or the declination of the center of each astrographic plate deg PLATE plate identifier running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. --- HYPH hyphen number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- STAR running number of star on the plate number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- RAh right ascension (hours) [B1950] number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. h RAm right ascension (minutes) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. min RAs ascension (seconds) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. s DE- declination sign number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- DEd declination (degrees) [B1950] number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. deg DEm declination (minutes) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. arcmin DEs declination (seconds) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. arcsec EPOCH plate epoch number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. a mB photographic magnitude number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. mag AGKNO AGK2 number AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- SUFFIX suffix to the AGK2 number Suffix to the AGK2 number, if needed, otherwise CR/LF. number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= Suffix to the AGK2 number, if needed, otherwise CR/LF. --- ZONE plate identifier declination zone, or the declination of the center of each astrographic plate deg PLATE plate identifier running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. --- HYPH hyphen number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. --- STAR running number of star on plate Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. --- RAh right ascension (hours) [B1950] number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. h RAm right ascension (minutes) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. min RAs right ascension (seconds) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. s DE- declination sign number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. --- DEd declination (degrees) [B1950] number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. deg DEm declination (minutes) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. arcmin DEs declination (seconds) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. arcsec EPOCH plate epoch number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. a mB photographic magnitude number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. mag AGKNO AGK2 number, if AGK2/3 star was AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. --- SUFFIX suffix to the AGK2 number suffix to the AGK2 number, if needed, otherwise CR/LF. number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that zones lower from 27 deg have generally 180 plates, and those higher from 28 deg have 160 plates. number= Note that this number in the Oxford I zone is so determined to be unique in a whole zone (e.g., in the zone +25 deg.). number= AGK2 number, if AGK2/3 star was identified, otherwise CR/LF. Note that this is incomplete. number= suffix to the AGK2 number, if needed, otherwise CR/LF. --- J.A. Watko SSDOO/ADC 1995 Koichi Nakajima [CDS] 24-Sep-1993 Nov 16 I_21A.xml 1022A I/22A Astrographic Catalogue Algier, -02 to +04 P Lacroute A Valbousquet CDS Bull. No. 6, p. 38 ??? ??? 1974 1974BICDS...6...38L Positional data Astrographic zones Magnitudes, photographic The "Carte de Ciel" (or "Astrographic Catalogue") is a catalogue of star positions and magnitudes, determined on the photographic plates taken by the normal astrographs which are installed in observatories of various latitudes, as a world-wide astronomical project (see Eichhorn, 1974, p279). The catalogue is divided into 22 declination zones, each of which is assigned to each observatory, e.g., a zone from +18 to +24 degrees is to Paris observatory. Each observatory has taken photographs of 2 deg x 2 deg area in and covering each zone, measured the X,Y coordinates of star images on the photographic plates, and published the results as the printed catalogues. The present catalogue is the results of reduction of these X,Y coordinates into right ascension and declination values, for declination zones of +05 to +31, by using AGK2/3 catalogue as the reference.

ZONE plate identifier declination zone, or the declination of the center of each astrographic plate deg PLATE plate identifier running number of plate in the zone Note that this number is negative when the zone is negative. --- STAR running number of star on the plate number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. --- RAmas right ascension (B1950) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. mas DEmas declination (B1950) number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. mas EPOCH plate epoch from 180000 number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. ca mB photographic magnitude number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. dmag X X coordinate on the plate number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. 0.1um Y Y coordinate on the plate number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. 0.1um AGK3Z AGK3 number : zone number No signs on any AGK3 zones. number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. deg AGK3N AGK3 number : star number number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. --- ZERO zero number= declination zone, or the declination of the center of each astrographic plate number= running number of plate in the zone Note that this number is negative when the zone is negative. number= No signs on any AGK3 zones. --- Koichi Nakajima CDS 1993 J.A. Watko [SSDOO/ADC] 21-Feb-1996 Sep 24 I_22A.xml 1040 I/40 WASHINGTON 20 Catalog H R Morgan Publ. USNO, 2nd series, vol. XIII, Washington ??? ??? 1933 1983 Meridian observations Positional data Historical catalog This catalogue contains the two parts: the 9989 first stars are the standard and intermediary stars, +90 to -36 degrees of declination, observed in the years 1913 to 1926, and reduced without proper motion to the equinox 1920.0 ; the second part (stars numbered 9990 to 10571) are 582 miscellaneous stars.

Seq Running number --- DM Durchmusterung (BD or CD) identification --- Sp Spectral type, from HD --- NumSp Coded spectral type number=1 the numeric spectral type exists only for stars 1-10400; it is coded on 3 bytes as follows: ------------------------------- Byte#16 Byte#17 Byte#18 ------------------------------- R=0 a or 0=0 Oe5=1 b or 1=1 O=2 c or 2=2 B=2 d or 3=3 *=3 A=4 e or 4=4 F=5 5=5 e=5 G=6 6=6 K=7 7=7 M=8 8=8 N=9 9=9 S=- p=- ------------------------------- Special cases: Mb=83 Mc=88, Md=8 5, Me=8-5, Np=9 --- Vmag Magnitudes (from Harvard Revised Photometry or corrected BD) mag n_Vmag for variable star --- ObsMag Observed magnitude mag RAh Right Ascension B1920 (hours), at Epoch h RAm Right Ascension B1920 (minutes), at Epoch min RAs Right Ascension B1920 (seconds), at Epoch s pmRA Annual proper motion in RA (in Boss system) s/a DE- Declination B1920 (sign) --- DEd Declination B1920 (degrees) deg DEm Declination B1920 (minutes) arcmin DEs Declination B1920 (0.01arcsec) arcsec pmDE Annual proper motion in Dec (in Boss system) arcsec/a o_RAs Number of observations in RA --- o_DEs Number of observations in Dec number=2 the value is not specified when it is identical to the corresponding number for RA. --- EpRA-1900 Mean Epoch of Right Ascension 0.01a EpDE-1900 Mean Epoch of Declination number=2 the value is not specified when it is identical to the corresponding number for RA. 0.01a Note indicates a note in the catalog --- Francois Ochsenbein, James Marcout CDS 1998 Jun 10 UNKNOWN UNKNOWN The catalogue was originally keypunched at the Astronomisches Rechen-Institut, Heidelberg, Germany, in the 70's. It contained 10400 stars, i.e. 171 stars were missing (note from Richard Swifte, Royal Greenwich Observatory, October 1981). The missing stars were added in June 1998, with the help of an Optical Character Recognition system. I_40.xml 1044 I/44 Second Cat of Fundamental Stars G D Baturina V S Bedin K G Gnevysheva M S Zverev A A Naumova A I Plugina D D Polozhentsev T A Polozhentseva E A Stepanova Tr. Glav. Astron. Obs. Pulkovo, ser. 2 86 4-158 1986 1986TrPul..86....4B Positional data The Catalogue SPF2 was obtained from observations of the fundamental FK4 stars as a reference stars for SRS, BS and DS star. Observations were made by Pulkovo observers in the declination zone -42 to -90 and +16 to -16 degrees using Repsold Meridian Circle of the Cerro Calan Observatory (Santiago, Chile) from 1963 to 1968.

They worked in closed cooperations with their Chilean colleagues who observed other declination zones. In total 15160 observations were made of FK4 stars. The reductions of observations were made by the quasi-absolute method proposed by M.S.Zverev (1969). Investigations were carried out of the systematic differences of type "E-W" as well as of the personal equations. Also differences of type "Upper - Lower culmination" were investigated. All these corrections were applied to the observations. The mean error of the single observations reduced to the equator is +/- 14.0 millisecond of time. The mean error of the position of a single star reduced to the equator is +/- 2.8 millisec of time (each position in the middle are consists from 25 observations). The main results of the systematic errors were published by Zverev and Naumova.

03 "03" --- ID FK4 number --- mag Magnitude mag RAh Right Ascension (B1950.0) hours h RAm Right Ascension (B1950.0) minutes min RAs Right Ascension (B1950.0) seconds s DE- Declination (B1950.0) sign --- DEd Declination (B1950.0) degrees deg DEm Declination (B1950.0) arcminutes arcmin DEs Declination (B1950.0) arcsec arcsec del_RA RA-RA(FK4) s Ep Epoch of mean observation - 1900 years a e Error E*cos(DE) where E = error of observations s N Number of observations --- rem Remark "-3" data of spf2b.dat exist "03" data of spf2b.dat do not exist --- ID FK4 number --- mag Magnitude mag RAh Right Ascension (B1950.0) hours h RAm Right Ascension (B1950.0) minutes min RAs Right Ascension (B1950.0) seconds s DE- Declination (B1950.0) sign --- DEd Declination (B1950.0) degrees deg DEm Declination (B1950.0) arcminutes arcmin DEs Declination (B1950.0) arcsec arcsec del_RA RA-RA(FK4) s Ep Epoch of mean observation - 1900 years a e Error E*cos(DE) where E = error of observations s N Number of observations --- 3 "3" --- ID FK4 number --- mag Magnitude mag RAh Right Ascension (B1950.0) hours h RAm Right Ascension (B1950.0) minutes min DE- Declination (B1950.0) sign --- DEd Declination (B1950.0) degrees deg DEm Declination (B1950.0) arcminutes arcmin uRA RA-RA(FK4) (upper culmination) s uEp Epoch of mean obs (upper culmination) - 1900 a ue Error (upper culmination) s uN Number of observations (upper culmination) --- lRA RA-RA(FK4) (lower culmination) s lEp Epoch of mean obs (lower culmination) - 1900 a le Error (lower culmination) s lN Number of observations --- Nancy Grace Roman and Julie Anne Watko SSDOO/ADC 1996 Feb 29 We appreciate the extensive information provided by D. Polojentsev. I_44.xml 1061B I/61B AGK3 Catalogue W Dieckvoss O Heckmann Hamburg-Bergedorf ??? ??? 1975 1975QB6.A15.......D I/176 : AGK3U: an updated version of the AGK3 (Bucciarelli+ 1992) I/69 : AGK3 Catalogue by Right Ascension (Dieckvoss, Heckmann 1975) I/161 : AGK3R (Smith 1990) Cannon, A. J. (1925-1936), The Henry Draper Extension, Ann. Astron. Obs. Harvard College 100. Cannon, A. J. and Pickering, E. C. (1918-1924), The Henry Draper Catalogue, Ann. Astron. Obs. Harvard College 91-99. Dieckvoss, W. (in collaboration with H. Kox, A. Gunther and E. Brosterhus) (1975), AGK3 Star Catalogue of Positions and Proper Motions North of -2.5 Degrees Declination, Hamburg-Bergedorf. Nagy, T. A. 1979, Documentation for the Machine-Readable Version of the AGK3 Catalogue of Positions and Proper Motions North of -2.5 Degrees Declination, Systems and Applied Sciences Corporation R-SAW-7/79-35. Warren, W. H. Jr. and Kress, K. 1980, Astron. Data Center Bull. 1, 19. Willstrop, R. V. 1983, Bull. Inf. Cent. Donnees Stellaires No. 24, 65. Positional data Proper motions Magnitudes, photographic The AGK3 provides positions and proper motions for stars north of -2.5 degrees. For the most part, it contains the stars in the AGK2 but is based on newly remeasured reference stars whose positions were reduced to the FK4 system. A list of 446 AGK2 stars not in the AGK3 and of three new stars is provided. All plates were taken at the Bergedorf Observatory. In addition to the positions and proper motions, the catalog contains magnitudes and spectral types, the epoch of the observations, the epoch difference between the AGK2 and AGK3, and the BD numbers.

The AGK3 Star Catalogue of Positions and Proper Motions North of -2.5 Degrees Declination (hereinafter AGK3) was conceived and planned during discussions between O. Heckmann and D. Brouwer at Hamburg Observatory following the 1952 International Astronomical Union (IAU) General Assembly in Rome. It was concluded that an adequate number of reference stars (AGK3R) should be observed by as many meridian circles of as many observatories as possible, the revision of FK3, then in progress (FK4), should define the reference frame, and the same instruments as used for AGK2 should be used for the observations for AGK3. A formal recommendation was adopted through Commission 8 at the 1955 IAU General Assembly in Dublin, with the observatories at Babelsberg, Bergedorf, Bordeaux, Greenwich, Heidelberg, Nikolajew, Ottawa, Paris, Pulkovo, Strasbourg and Washington (USNO) to collaborate in the work, and with F. P. Scott (USNO) to coordinate the meridian circle observations of AGK3R stars. The completion of the photographic observations was to be the responsibility of the observatories at Bergedorf and Bonn, with all plate measurements to be done at the former. (However, it was finally decided that all plates, even for the AGK2 Bonn zones, would be taken at Bergedorf.) The plates for AGK3 were secured at Bergedorf between August 1956 and June 1964, with special precautions (exposures on both sides of the pier) made to compensate for possible changes in the camera objective. The two sets of plates were measured at Bergedorf in opposite directions and averaged to obtain final x,y coordinates. The detailed procedures for the correction of magnitude-color errors, reduction of the measures using the AGK3R stars, re-reduction of AGK2 using its reference catalog AGK2A transformed to the FK4 system, and final reduction of the AGK3 positions and proper motions, are discussed by W. Dieckvoss in his technical introduction to the source reference. Although a more detailed discussion of errors is given by Dieckvoss, the standard error for one coordinate on one plate as determined from a limited sample of 110 pairs of plates is +/- 0.025" for AGK3.

AGsign Sign of AGK3 number. --- AGzone AGK3 zone. --- AGnum AGK3 number AGK3 number in increasing order within each declination zone. The field is filled with preceding zeros. --- m_AGnum Component for duplicates Component identification where duplicates AGK3 numbers occur. The lower case letters "a" and "b" may be present. --- Pmag Photographic magnitude from AGK2 mag Sp Spectral type Spectral Type from Henry Draper Catalogue (Cannon and Pickering, 1918-1924), its Extension (Cannon, 1925-1936), Schildt (Yale Transactions) or determined by A. N. Vyssotsky and collaborators at the Leander-McCormick Obs. --- RAh Right ascension hours (1950.0) h RAm Right ascension minutes (1950.0) min RAs Right ascension seconds s DE- Sign of declination (1950.0) --- DEd Declination degrees (1950.0) deg DEm Declination minutes arcmin DEs Declination seconds arcsec nobs Number of photographic observations Number of photographic observations used to determine the position. Single-digit numbers are preceded by a zero. --- Ep-1900 Epoch of AGK3 position minus 1900 yr pmRA Annual proper motion in right ascension Annual proper motion in right ascension multiplied by cos(delta), determined by differencing the AGK3 and AGK2 positions and dividing by the epoch difference. Proper motions are missing for stars new in AGK3 (see Table 6). If a calculated value of the proper motion exceeded the field capacity a value of "9999" is given with a "+" in byte 38. The suggested format reads the datum in the correct units. mas/yr pmDE Annual proper motion in declination mas/yr dEpoch Epoch difference AGK3-AGK2 yr BD Full BD catalog designation The full BD identification (see cat. <I/122>) contains: bytes 59-60: "BD" or blank byte 61: Sign of BD zone number bytes 62-63: BD zone number bytes 64-68: BD number within zone --- m_BD Component of multiple system Numerical code for identification of a component of a multiple system: (1 = primary [P]; 2 = secondary [S]; 3 = A; 4 = B; 5 = S1; 6 = S2; 7 = P1; 8 = P2; 9 = C). BD supplemental stars (lower case letters) are assigned codes but are indistinguishable from A and B designations because the codes are the same. Since the file format only allows one byte for the duplicity code, and nine codes are already used, the distinction cannot be drawn. If it is necessary to distinguish or identify supplemental stars, the Catalog of BD Supplemental Stars (Warren and Kress 1980) should be used. --- Sum Sum of discrepancy codes Sum of discrepancy codes, calculated as the sum of 2**v (2 to the power of v), where v = 0 (BD number), 1 (mpg and/or spectral type), 2 (AGK2 right ascension), 3 (AGK2 declination), 4 (AGK3 right ascension), 5 (AGK3 declination). --- pmsec Annual proper motion in seconds of RA, computed by dividing by 15cos(delta) s/yr dRA The difference in right ascension in the sense AGK3 - AGK2modified The residual quantity of the difference in right ascension (multiplied by cos(delta)) in the sense AGK3 - (AGK2modified), where the last quantity denotes data from the re-reduced AGK2. arcsec dDE The difference in declination in the sense AGK3 - AGK2modified arcsec agk3.doc Documentation James E. Gass and Gail L. Schneider SSDOO/ADC 1997 Jul 01 UNKNOWN UNKNOWN The machine version of the AGK3 was received on magnetic tape from the Centre de Donnees Stellaires, Strasbourg in 1978. The version received had been obtained originally from the Astronomisches Rechen- Institut in Heidelberg. A preliminary document for a modified and corrected version of the catalog was produced by Nagy (1979). The following changes were made to the Heidelberg file in order to correct some minor errors and to produce a file conforming more closely to the published version: 1. AGK3 component identifications for stars where more than one AGK3 star has the same number were changed from upper case characters (A, B) to lower case (a, b) as in the printed edition. 2. Nine stars in AGK3 zone -00, but in BD zone +00 were found to have a BD zone of +90. The BD zone for these stars was changed to +00. These stars are: AGK3 -00 1467, 1510, 1530, 1531, 1532, 1602, 1693, 1774, and 2120. 1-Jul-1997: Explicit decimal points added to floating point fields in computer-readable version. Document brought up to standard. [J. Gass, ADC] 1-Sep-1998: filled blanks between sign and value with zeroes in columns pmRA, pmDE, pmsec, dRA, dDE to allow correct interpretations [F. Ochsenbien, CDS] I_61B.xml 1062C I/62C Perth 70 B: Positions 24900 Stars E Hog J von der Heide Abh. der Hamberger Sternwarte, Band IX. ??? ??? 1976 1976AAHam...9....1H Astrometric data Photometry This Perth 70: A Catalogue of Positions of 24900 Stars contains accurate positions and magnitudes of 24,871 reference stars, mostly in the southern hemisphere, plus other useful data such as approximate proper motions, radial velocities, and parallaxes. The Perth 70 is a result of meridian circle observations made by the Hamburg Observatory expedition to Perth as part of the international effort on Southern Reference Stars (SRS). The catalog described here provides the mean values for each star, including the position, magnitude, and mean epoch of observation; the proper motions, however, were neither observed nor recomputed from comparing the Perth positions to older material.

This catalog is the September 1992 version of the results of meridian circle carried out at Perth in the late 1960's and early 1970's. Some 107 circumpolar stars occupy two records each, one for observations at upper culmination and one for observations at lower culmination, so the number of records is greater than the number of stars. This file contains the mean values of the meridian circle observations (position and magnitude) made at Perth, plus auxiliary quantities usually taken from the preliminary version of the Southern Reference Stars (SRS) catalog (Corwin, 1992). The first part of each record presents the same information that is contained in the printed catalog; the remaining information was not printed. Missing data are denoted by blank-filled fields except for the standard errors of one observation in R.A. * cos(dec) and in declination. In those fields, missing data are indicated by "0". Stars with numbers in the 30000's are in the FK4 catalog, with the last four digits being the FK4 number. Stars with numbers in the 40000's are in the Bright Star Catalog in the same format. Stars with other numbers are program stars.

ID Perth 70 catalog number --- n_ID S means star is in the FK4 suppl. --- V V magnitude If the hundredths place (byte 12) is blank, the number was copied from the preliminary SRS; otherwise, the magnitude was observed at Perth. mag Sp Spectral type; from SRS The spectral types are always those of the printed catalog. Two stars must be mentioned specifically: fl2 Velorum (SRS #30309) and O Cygni (SRS #44262). The first, a Wolf-Rayet star (type WC), is listed in the FK5 as "Oap" (the HD designation) and appears here as "O0." The second, a Mira Ceti-type pulsating variable, spectral type "S7ev," appears here as "M7." --- RAh Right ascension hours (B1950) Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. h RAm Right ascension minutes (B1950) Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. min RAs Right ascension minutes (B1950) Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. s cul Culmination flag This is blank except for circumpolar stars, which have 2 records, one marked `U' for upper culmination observations, and one marked `L' for lower culmination observations. --- DE- Sign of declination --- DEd Declination degrees (B1950) deg DEm Declination minutes (B1950) arcmin DEs Declination seconds (B1950) arcsec epRA Mean epoch of observation in RA -1900000 Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. ma epDE Mean epoch of observation in dec -1900000 ma o_RA Number of observations in RA Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. --- RAdel Indicates >=1 obser. in RA deleted Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. --- o_DE Number of observations in declination --- DEdel Indicates >=1 obser. in dec deleted --- q_RAs Residual in right ascension Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. These are the Perth position minus the position in the preliminary SRS, corrected for proper motion to the mean epoch of observation. The signs of the residuals are changed for circumpolar stars observed at lower culmination. carcsec q_DEs Residual in declination carcsec pmRA Proper motion in right ascension Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. These are copied from the preliminary SRS; the Perth 70 positions were not used to compute them. For centennial proper motions, use formats F7.3 and F7.2 for proper motion in RA and proper motion in declination, respectively. s-5/a pmDE Proper motion in declination These are copied from the preliminary SRS; the Perth 70 positions were not used to compute them. For centennial proper motions, use formats F7.3 and F7.2 for proper motion in RA and proper motion in declination, respectively. arcsec-4/a DMcat Durchmusterung catalog The catalog identifier (bytes 84-85) is either `BD' for Bonner Durchmusterung, `CD' for Cordoba Durchmusterung, or `CP' for Cape Photographic Durchmusterung. The zone is contained in bytes 87-89 (with the sign in byte 87), and the serial number, in bytes 90-94. --- DMzone Durchmusterung zone --- DMnum Durchmusterung number --- type Type of star One of `P' for program star, `F' for FK4 star, or `B' for Bright Star Catalog star. --- obs_no Observing number for part A This number is included to enable cross references between this catalog and Part A; it does not appear in the printed catalog and should not be used as the principal identification number. Circumpolar stars have distinct observing numbers for upper and lower culmination. (Part A lists the individual observations.) --- o_obs_no Number of records in part A --- n_n_ID FK4 Supplement number --- RV Radial Velocity dkm/s Plx Parallax marcsec o_V Number of observations of magnitude --- n_V Indicates >=1 obser. in V deleted --- mean Mean epoch of observation in V -190000 ca e_RAs Standard error of one obs. in RA*cos(dec) Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. carcsec e_DEs Standard error of one obs. in declination carcsec e_V Standard error of one obs. in magnitude cmag n_PlxRA Mean parallax factor in right ascension Positions are referred to the system of the FK4 (equinox B1950.0) at the mean epoch of observation for each coordinate for each star. carcsec n_PlxDE Mean parallax factor in declination carcsec pre_V V magnitude from preliminary SRS cat. The preliminary SRS positions may be recovered by RA SRS =RA Perth-PM RA(t RA-1950)+/-(delta RA cos(dec))=15cos(dec SRS) dec SRS = dec Perth-PM dec(t dec-1950)+/-delta dec where t is the mean epoch for the coordinate. The plus sign is taken only for stars observed at lower culmination. The factor 15 in the first equation emphasizes that ff cosffi is tabulated in arc seconds whereas right ascension is customarily expressed in units of time. mag newperth.doc The original more detailed ADC document N. G. Roman SSDOO/ADC 1997 May 27 I_62C.xml 1068A I/68A Positions and Proper Motions in alpha Per cluster A Fresneau Bull. Inform. CDS 18 81 1980 1980BICDS..18...81F Positional data Proper motions Regional catalog A list of positions and proper motions is given for 2027 stars of magnitude 7.5 to 12.5 within a radius of 3.5 deg. of alpha Persei. The values are poor for stars fainter than 11. The present list supersedes the microfiche edition (catalogue I/68/) which was described in the Bull. Inform. CDS 18, 81 (1980).

Mel20 Heckmann's number number as published in Astron. Nachr. 283, 109 (Mitt. Hamburger Sternw. 1956MiHam..10...37H) if the star belongs to Heckmann's list --- BD BD (cat. <I/122>) or CSI (Catalogue of Stellar Identifications) this identification is not in BD when a dash (-) follows the degree zone number. --- SpType Spectral type (from Heckmann) --- Pmag Photographic Magnitude, in 0.1 magnitude 0.1mag Epoch Epoch of equatorial coordinates yr RAh RA 1950 at Epoch (hours, always 3) h RAm RA 1950 at Epoch (minutes) min RAs RA 1950 at Epoch (seconds) s e_RAs Mean error on RA (seconds) a zero mean error means that only one observation is available, and hence the mean error is undefined. s pmRA Proper motion mu_alpha in time seconds/century s/ha e_pmRA Mean error on pmRA s/ha DE- Declination 1950 at Epoch (sign) --- DEd Declination 1950 at Epoch (Degrees) deg DEm Declination 1950 at Epoch (Arc minutes) arcmin DEs Declination 1950 at Epoch (Arc seconds) arcsec e_DEs Mean error on Dec (arc seconds) arcsec pmDE Proper motion mu_delta in arcsec/century arcsec/ha e_pmDE Mean error on pmDE arcsec/ha Alain Fresneau, Francois Ochsenbein Strasbg Obs. 1993 Mar 26 I_68A.xml 1069 I/69 AGK3 Catalogue by Right Ascension W Dieckvoss O Heckmann Hamburg-Bergedorf ??? ??? 1975 1975QB6.A15........ Positional data Proper motions Magnitudes, photographic The AGK3 catalog of positions and proper motions is a photographic catalog based on plates taken with the same instruments as the AGK2 and referred to a network of meridian observations (the AGK3R). The AGK2 positions were rereduced using its reference catalog, AGK2A, reduced to the FK4 system. The positions and motions are on the FK4 system. The positional errors in one coordinate are about 0.025". Information contained in the catalog includes in addition to the positions and proper motions in the B1950 system, the AGK3 zone and number, a component identification when duplicate AGK3 numbers occur, photographic magnitude, spectral type, number of photographic observations used to determine the position, epoch of the position, epoch difference: AGK3 - AGK2 and the DM number and component.

AGK- Sign of AGK3 number. --- ZONE AGK3 declination zone. --- ID AGK3 number in order within zone. --- DUP Component id for duplicate numbers. number=1 The lower case letters "a" and "b" may be present if there are multiple components, otherwise there is a "0". --- mpg Photographic magnitude. number=2 Taken from AGK2. mag Sp Spectral type. number=3 Adopted from the Henry Draper Catalogue (Cannon and Pickering 1918-1924), its Extension (Cannon 1925-1936), Schildt (Yale Transactions) or determined by A. N. Vyssotsky and collaborators at the Leander-McCormick Obs. --- RAh Right ascension (hours) (Equinox 1950.0). h RAm Right ascension (minutes) min RAs Right ascension (seconds) s DE- Sign of declination (Equinox 1950.0). --- DEd Declination (degrees) deg DEm Declination (arcminutes) arcmin DEs Declination (arcseconds) arcsec Num Number of photographic observations used to determine the position. --- Epoch Epoch of AGK3 position - 1900. a pmRA- Sign of proper motion in right ascension. --- pmRA Proper motion in right ascension. number=4 Multiplied by cos(DEC), determined by differencing the AGK3 and AGK2 positions and dividing by the epoch difference. Proper motions are missing for stars new in AGK3 (see Table 6). If a calculated value of the proper motion exceeded the field capacity a value of "9.999" is given with a "+" in byte 38. arcsec/a pmDE- Sign proper motion in declination. --- pmDE Proper motion in declination. number=4 Multiplied by cos(DEC), determined by differencing the AGK3 and AGK2 positions and dividing by the epoch difference. Proper motions are missing for stars new in AGK3 (see Table 6). If a calculated value of the proper motion exceeded the field capacity a value of "9.999" is given with a "+" in byte 38. arcsec/a SepEp Epoch difference AGK3-AGK2. a BD- Sign of zone number --- BD BD catalog designation --- BDZONE BD zone. --- BDNum BD number within zone. --- pmRAt- Sign of right ascension proper motion. --- pmRAt Proper motion in right ascension. number=5 In units of seconds of time per year. Computed by dividing by 15cos(delta). s/a d(RAmod)- Sign of right ascension difference. --- d(RAmod) Residual quantity of the difference. number=6 Residual in right ascension (multiplied by cos(delta)) in the sense AGK3 - (AGK2modified), where the last quantity denotes data from the re-reduced AGK2. arcsec d(DEmod)- Sign of declination difference. --- d(DEmod) Residual quantity of the difference. number=7 Residual in declination in the sense AGK3 - (AGK2modified). arcsec agk3_ra.doc Original ADC documentation Edward J. Shaya SSDOO/ADC 1997 Jul 15 I_69.xml 1071 I/71 Bonner Durchmusterung Supplemental Stars W H Warren Jr. K Kress unpublished ??? ??? 1980 1980 Durchmusterungen The Bonner Durchmusterung catalogs (Argelander 1859-62, Kuestner 1903), declination zones +89deg. to -01deg., contain supplemental stars having lower case letter designations following the BD numbers after which they have been inserted. Many problems of identification have arisen over the years because the supplemental stars have been included in certain machine-readable catalogs without their letter designations, thus making it impossible for a computer to distinguish between a BD star and its insert(s). The need for a machine-readable version of the supplemental stars arose in connection with identifying stars in other catalogs in order to add the letter designations to them. The initial catalog of supplemental stars was prepared from the second edition of the BD (Kuestner 1903), but proofreading and checking were accomplished by using the reprinted edition (Bonn Universitaets Sternwarte 1968) which incorporated all errata known at that time. In that way, it was possible to simultaneously derive tables of supplemental stars added, deleted, or modified for the reprinted edition. The machine-readable version of the Catalog of Supplemental Stars to the Bonner Durchmusterung is a compilation of Bonner Durchmusterung stars having lower case letter designations in the original published edition of the catalog. The data include all information given in the original published edition as footnotes except for the old spectral types sometimes reported there.

BDs BD number sign --- BDz BD zone --- BDno BD number within zone BD numbers are determined by the position of the footnoted star in the original published catalog. --- let Letter designation --- RAh Right ascens.(1855)hours Equinox 1855. h RAm Right ascen.(1855)min Equinox 1855. min RAs Right ascen.(1855)sec Equinox 1855. 0.1s RAds Right ascen.(1855)decisec Equinox 1855. ds DE- Sign of declination (1855) --- DEd Declination (1855) degrees deg DEm Declination (1855) minutes 0.1arcmin DEdm Declination (1855) decimin darcmin mag Magnitude Magnitudes are visual and were taken directly from the published catalog. mag Nancy G. Roman ADC/SSDOO 1995 Jun 13 The original document for this catalog was prepared in Script by Wayne H. Warren Jr. It was translated to ASCII and put into the current standard form by the undersigned. The only other change was to fill blanks in the position coordinates with zeros to facilitate proper reading. UNKNOWN UNKNOWN The original BD supplemental data were transferred to coded forms by K. Kress at the National Space Science Data Center (NSSDC), NASA Goddard Space Flight Center. They were also transferred to punched cards at NSSDC, and thence to a computer disk file accessible via an interactive system. The listed file was then proofread against the reprinted microversion (Bonn Universitaets Sternwarte 1968) and additions, deletions, and modifications were made to the file by W. H. Warren Jr. All letter designations are coded as lower case characters just as they appear in the original published catalog. The order of the stars in the catalog is from north to south and increasing right ascension within each declination zone. The magnitude data must be read in character format because the words VAR and NOV occur within the field and byte 27 contains a ? in one case. Tables 1-3 list stars that were either added, deleted, or had their designations changed in the 1968 reprinted edition of the BD. These lists enable the user to resolve differences between this catalog of supplemental stars and the 1903 edition of the published catalog, which is much more widely available than the 1968 edition. Table 1 Stars Added in Reprinted Edition ------------------------------------------------------------------------------- -00 2281a +26 1414a +35 180a +42 3093a +45 3139a +48 3799a -00 3110a +26 2056a +36 4154a +42 4100a +45 3141a +49 80a -00 4212a +26 2059a +37 3418a +42 4178a +46 489a +49 937a +00 4718a +28 258a +39 4869a +42 4611a +46 499a +49 1405a +02 2309a +28 1280a +40 260a +43 1164a +46 2755a +49 1571a +03 1727a +28 4536a +40 2004a +43 1784a +46 2844a +49 2117a +04 2289a +29 3503a +40 2006a +43 2563a +46 2886a +49 3452a +04 3561a +29 4240a +40 3209a +43 3248a +46 2912a +49 3546a +05 462a +29 4470a +40 4729a +43 3913a +46 3116a +49 4309a +12 206a +30 420a +41 312a +43 4086a +46 3934a +50 242a +15 4266a +30 4456a +41 1607a +43 4119a +47 630a +50 1907a +16 4370a +31 366a +41 1608a +43 4388a +47 1278a +56 606a +17 2116a +31 2042a +41 2269a +44 312a +47 3074a +56 2616a +18 368a +32 4341a +41 2680a +44 1308a +47 3202a +57 2864a +18 3421a +32 4668a +41 2680b +44 2480a +48 1302a +58 764a +19 339a +33 21a +41 3640a +44 2721a +48 1391a +58 1096a +21 1842a +33 1429a +42 376a +44 3419a +48 1538a +59 2826a +21 2355a +33 4238a +42 401a +45 513a +48 1783a +67 1046a +21 3114a +34 527a +42 1084a +45 1068a +48 1986a +76 857a +23 1503a +34 666a +42 1798a +45 1073a +48 2827a +78 314a +26 71a +34 4595a +42 2954a +45 1215a -------------------------------------------------------------------------------- Table 2 Supplemental BD Stars Deleted from Original Edition in Reprinted Edition -------------------------------------------------------------------------------- +13 5168a +15 612a +46 1767a -------------------------------------------------------------------------------- Table 3 Modifications of Original Supplemental Numbers in Reprinted Edition -------------------------------------------------------------------------------- +40 4729a changed to +40 4729b, +40 4729a added +48 1302a changed to +48 1302b, +48 1302a added -------------------------------------------------------------------------------- I_71.xml 1073B I/73B Sydney Photographic Cat 20457 Stars, -48 to -54 H Eichhorn W D Googe C F Lukac J K Murphy AJ 88 546 1983 1983AJ.....88..546E Positional data Photographic catalog This catalog is also known as the Sydney Photographic Catalogue -48 to -54 Degrees or SPC and gives positions determined by the plate overlap method from plates taken at the Sydney Observatory in 1964. The catalog was originally planned to fill part of the gap left by the Yale Zone and Cape Photographic Catalogues, although the gap has in the meantime been closed by catalogs prepared at Sydney Observatory (Nicholson 1979, King and Lomb 1983). Data in the catalog include star number (CPD; identifications not complete), source catalog identification (AC zones) and related information, right ascension/declination on the FK4 system (equinox and equator B1950, average epoch 1964.475), photovisual magnitude, and numbers of images and pairs of diffraction spectra used in computing position.

CPDnum Number in Cape Photographic Durchmusterung From Gill and Kapteyn (1897, 1900). The zone sign (always -) is in byte 1, the zone in bytes 2-3, byte 4 is blank, and the number is in bytes 5-9. The identifications are not complete, i.e., existing CPD numbers are not always present. --- Source Source catalog identification A Gill and Hough (1923) B Jackson and Stoy (1955) 1-120 Plates in Cape AC zone -49 deg 121-240 Plates in Cape AC zone -51 deg (Cape 1913-1926) 241-360 Plates in Sydney AC zone -53 deg (Sydney Obs. 1923-1933; see Wood 1971) where each AC zone is covered by 120 plates and 120 or 240 is subtracted to obtain plate numbers in the -51 deg and -53 deg zones, respectively. --- number Star or plate number in the source catalog --- refstar Asterisk (*) means the star served as a reference star. --- RAh Right ascension hours (1950) Given for the mean coordinate system 1950, ostensibly on the system of the FK4, at the average epoch 1964.475 of all plates which provided data. (If higher accuracy epochs are required, Table I of Eichhorn et al. 1983 should be consulted.) h RAm Right ascension minutes (1950) min RAs Right ascension seconds (1950) s DE- Sign of declination (1950) --- DEd Declination degrees (1950) deg DEm Declination minutes (1950) arcmin DEs Declination seconds (1950) arcsec Ptm Photovisual magnitude, taken from existing sources. For AC stars, the magnitudes were computed from data given in the AC and are photographic. Magnitudes are neither precise nor accurate and are given for reference purposes only. mag o_image Number of measured central images used to calculate the published position. --- o_spect Number of pairs of diffraction spectra used to calculate the published position. The number of individual images measured for computing a published position is the number in byte 51 plus twice the number in byte 53 (see Eichhorn et al. 1983). --- adc.doc ADC Documentation James E. Gass SSDOO/ADC 1997 Jul 31 Appreciation is expressed to Dr. H. Eichhorn for providing the SPC on tape and for reviewing and commenting on the original ADC document. UNKNOWN UNKNOWN The machine-readable version of the SPC was received on magnetic tape from records with bytes 1-25 blank and many other blanks throughout the records. The records on this tape had been designed specifically for printing the catalog and microfiching rather than for efficient storage and computing. To increase storage efficiency the following modifications were made after checking with the first author to be certain that the changes would be acceptable. 1. Superfluous blanks were removed from throughout the data records, except for a single separator blank between each of the data fields decreasing the logical record length from 104 to 53 bytes. 2. Leading zeros were added to all right ascension and declination fields. I_73B.xml 1078 I/78 SPF3 Catalogue P R Loyola V N Shishkina Publ. Dept. Astronomy Univ. of Chile 2 159 1974 1974PDAUC...2..159L I/82 : SPF1 Catalogue (Anguita et al., 1975, =1975PDAUC...2..181L) I/44 : SPF2 Catalogue (unpublished) Fricke, W. and Kopff, A., 1963, Fourth Fundamental Katalog (FK4), Veroeff. Astron. Rechen-Inst. Heidelberg, No. 10. (Catalogue: I/143) Morgan, H.R., 1952, "Catalog of 5,268 Standard Stars for the Equinox and Epoch 1950.0 Based on the Normal System N30", Astron. Papers Amer. Ephemeris 13, Part III. (Catalogue: I/13) Meridian observations Positional data Stars, fundamental The "Third Santiago-Pulkovo Fundamental Stars Catalogue (SPF3)" is a catalogue of right ascensions (the primary datum) of 671 fundamental bright stars, as measured with a Zeiss broken transit instrument at Cerro Calan Observatory in Chile. The observations were made in series consisting of 70 stars observed along the meridian from +42deg to the pole in upper culmination and from the pole to -70deg in lower culmination; the program consisted of 231 series of observations. In addition to the final reduced right ascensions for the program stars, the catalogue contains cross identifications to the N30 (Morgan 1952) and FK4 (Fricke et al. 1963) catalogues, visual magnitudes, approximate declinations (equinox 1950.0), mean epochs of the observations, and mean errors of the determined right ascensions. This document describes the machine-readable version of the SPF3 catalogue as distributed by the Astronomical Data Centers. It is intended to enable users to read and process the catalogue data without unnecessary problems and guesswork. The source reference should be consulted for details regarding the instrument characteristics, measurements, reductions, and comparisons with other catalogues.

SPF3 sequential number. --- FK4 FK4 (Fricke et al., 1963) --- N30/GC N30 or GC number (see byte 13). --- n_N30/GC Asterisk (*) if the N30/GC contains a GC identification; otherwise blank. --- Vmag Visual magnitude 0.01mag RAh Right Ascension 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAms Right Ascension 1950 (milli-seconds) ms DE- Approximate Declination 1950 (sign) --- DEd Approximate Declination 1950 (degrees) deg DEdm Approximate Declination 1950 (deci-minutes) 0.1arcmin EpRA Mean epoch for right ascension observations 0.01yr o_RAms Number of observations --- e_RAms Mean error of RAms ms Dimitri Polojentsev Pulkovo Francois Ochsenbein CDS 1995 Sep 18 Appreciation is expressed to Dr. A. Gutirrez-Moreno of the Universidad de Chile for supplying the published catalogue in printed form, and to M.H. Warren for proofreading the machine-readable version. UNKNOWN UNKNOWN * May 1982: The SPF3 catalogue was keyed directly to disk storage and proofread at the Astronomical Data Center, NASA Goddard Space Flight Center. File documented by Wayne H. Warren Jr., as document NSSDC/WDC-A-R&S 82-17 * 18-Sep-1995: documented with CDS standards; transformed epochs initially starting at 1950.00 I_78.xml 1079 I/79 Lowell Proper Motion Survey 8991 Northern Stars H L Giclas R Burnham Jr. N G Thomas Lowell Obs., Flagstaff, AZ ??? ??? 1971 1971lpms.book.....G I/112 : Southern Hemisphere Lowell Proper Motion Catalog (Giclas+ 1978) Giclas, H. L. 1958, Lowell Obs. Bull. 4, 1 (No. 89). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1961, Lowell Obs. Bull. 5, 61 (No. 112). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1963, Lowell Obs. Bull. 6, 1 (No. 120). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1964, Lowell Obs. Bull. 6, 103 (No. 122). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1964, Lowell Obs. Bull. 6, 135 (No. 124). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1965, Lowell Obs. Bull. 6, 197 (No. 129). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1966, Lowell Obs. Bull. 6, 233 (No. 132). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1966, Lowell Obs. Bull. 6, 271 (No. 136). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1967, Lowell Obs. Bull. 7, 1 (No. 138). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1967, Lowell Obs. Bull. 7, 31 (No. 140). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1968, Lowell Obs. Bull. 7, 67 (No. 144). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1969, Lowell Obs. Bull. 7, 129 (No. 150). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1970, Lowell Obs. Bull. 7, 149 (No. 151). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1970, Lowell Obs. Bull. 7, 165, (No. 152). Giclas, H. L., Burnham, R. Jr. and Thomas, N. G. 1971, Lowell Proper Motion Survey, Northern Hemisphere, The G Numbered Stars (Flagstaff: Lowell Observatory). Giclas, H. L., Slaughter, C. D. and Burnham, R. Jr 1959, Lowell Obs. Bull. 4, 136 (No. 102). Positional data Proper motions The catalog contains a summary of many individual papers published in the Lowell Observatory Bulletins in the years 1958 to 1970. The data in the machine-readable version include observed positions, proper motions, estimated photographic magnitudes and colors, and references to identifications in other catalogs. Photoelectric data on the UBV system are included for many stars, but no attempt was made to find all existing photometry. The notes.dat file was computerized at the ADC by keying the notes directly to disk storage.

G Original G number assigned Original G number assigned to the star on the plate region where it was first Found. Stars which were subsequently found on later plates were assigned new G numbers; however, in this catalog all duplicate observations have been combined and averaged with the original G numbers retained. Byte 1 of the field always contains a "G" and byte 5 always always contains a "-". The number in bytes 2-4 is the plate number, while that in bytes 6-8 is the star number on the plate. --- RAh Right ascension 1950 (hours) Epochs are given for plate regions in the original Lowell Bulletin numbers reported in the CHT column of the published catalog. h RAm Right ascension 1950 (minutes) min RAs Right ascension 1950 (seconds) s DE- Sign of declination --- DEd Declination 1950 (degrees) deg DEm Declination arcmin pm Annual proper motion arcsec/yr pmPA The position angle of proper motion PA of proper motion, measured in the normal way from North through East. deg Pmag Estimated photographic magnitude mag col Estimated color class Color class is on a scale of -1 (bluest) to +4 (reddest). Almost all stars having color class -1 have subsequently been classified as white dwarfs. An approximate relationship between estimated color and UBV colors is given in the published catalog. --- o_pm Number of observations Observations from different plate regions contained in the mean. A value of unity denotes a single observation from one plate pair. Actually, there are never as many as ten observations, so byte 33 is always blank. --- osource Or equivalent References for other sources containing information and/or data about the star. References are separated by blank characters and consist mainly of designations in other catalogs. A symbol "+" following the last reference indicates additional references in the notes to the catalog. The reference key is given in table2.txt. --- flag '*' indicates a note in file notes.dat Note in the published catalog which gives additional information about the star. See notes.dat for a description of the machine-readable notes. --- code Parallax Code Indicates if the star is on a parallax program of some observatory, thus denoting the possibility that a trigonometric parallax may eventually be be available. The following codes are employed: A Allegheny Obs. L Lick M Leander McCormick N U.S. Naval S Sproul V Van Vleck Y Yerkes A digit of >= 2 (= n) indicates the star to be on the working lists of n observatories. The codes for the n observatories are listed in table3.txt. --- Vmag Photoelectric V magnitude Photoelectric V magnitude obtained from the source given in bytes 95-97. UBV data are given for reference purposes only and no attempt for completeness has been made. Blank if no data reported. mag B-V B-V color (blank if no data) mag U-B U-B color (blank if no data) mag r_Vmag Ref code for the magnitude source The magnitude source reference key is given below. A digit >= 2 denotes multiple references (given in the notes.dat). Note: the appended minus signs on some codes are not explained in the published catalog. Lowell Proper Motion Survey, Northern Hemisphere. Magnitude Source Reference Key E1 Eggen, O. J. 1963, Astron. J. 68. 483. E2 Eggen, O. J. 1966, Royal Obs. Bull. No. 120. E3 Eggen, O. J. 1968, Astrophys. J. Suppl. 16, 97 (No. 143). E4 Eggen, O. J. 1969, Astrophys. J. Suppl. 19, 31 (No. 168). E5 Eggen, O. J. 1968, Astrophys. J. 153, 195. EG1 Eggen, O. J. and Greenstein, J. L. 1965, Astrophys. J. 141, 83. EG2 Eggen, O. J. and Greenstein, J. L. 1965, Astrophys. J. 142, 925. EG3 Eggen, O. J. and Greenstein, J. L. 1967, Astrophys. J. 150, 927. ES Eggen, O. J. and Sandage, A. 1967, Astrophys. J. 148, 911. G1 Greenstein, J. L. 1969, Astrophys. J. 158, 281. S1 Sandage, A. 1964, Astrophys. J. 139, 442. S2 Sandage, A. 1969, Astrophys. J. 158, 1115. SK Sandage, A. and Kowal, C. 1962, private communications. WG Gliese W. 1969, Catalogue of Nearby Stars, Veroff. Astron. Rechen-Inst. Heidelberg, No. 22. WA Wanner, J. F. 1964, Ph.D. Thesis, Harvard University. --- G G Star number, as in table north.dat --- m_G Shared note As described for bytes 1-8 in catalog.dat. If more than one consecutive G number is referred to, a slash (/) appears in byte 9 and the final digit of the second G number is given in byte 10. If more than two consecutive G numbers are included, a hyphen appears in byte 9 and the final digit of the last number in byte 10. A comma is given in byte 9 if two non-consecutive G numbers are referenced. Bytes 9 and 10 may also contain component identifications for double stars having the same G number, e.g. "AB". --- count Line counter Used to sequentially number remarks for the same star(s). Can be used as a secondary sort field to reorder the notes properly if they become disorganized. --- Text Text of remark --- table2.txt Key to reference abbreviations table3.txt Supplementary parallax codes Melissa C. Larkin SSDOO/ADC 1997 Mar 10 The original ADC documentation (1983) by Wayne H. Warren, Jr. was used to create this ReadMe file. He also did the original data reformatting. UNKNOWN UNKNOWN The first record in catalog.dat, containing only the word "MUCAT", was deleted. Multiple 80-byte records were combined while deleting a test digit in byte 80 indicating an additional record, and redundant G numbers on multiple records were removed. The machine-readable catalog contains 8989 records. A count of the stars in the published catalog (113 full pages with 75 stars per page and 68 stars on last page) gives 8993; however, stars are missing on pages 28, 29 and 42, resulting in 8989 stars total. Preceding zeroes were added to the G numbers to match the published catalog. There was no distinction between blank and 0.00 color indices. Initially, all zeroes were converted to blanks for B-V and U-B, then the published catalog was scanned for valid 0.00 values and the values were added for the appropriate stars. Plus signs were added to the declinations (byte 15), the color class positive values, and to all positive color indices. The following miscellaneous corrections to the published catalog were made to the machine file: G066-036 photoelectric data deleted as per published version G213-017 Declination degrees corrected from +39 to +37 G128-032 added BD+32 4584-5 The notes file was prepared by keying the published remarks directly to disk and adding to the catalog as a second file. I_79.xml 1080 I/80 Catalog of 5268 Standard Stars, Normal System N30 H R Morgan Astron. Papers Amer. Ephemeris 13, Part III ??? ??? 1952 1952N30...C......0M Positional data Proper motions Stars, fundamental Fundamental catalog The catalog was constructed primarily to assist in the reduction and interpretation of planetary observations, particularly those made in the nineteenth century. The new catalog was considered necessary because the only fundamental catalogs available at the time (FK3, GC) have mean epochs around 1900, and over the period of approximately fifty years, positional accuracies had deteriorated from cumulative effects of proper motion inaccuracies. The ADC version of the data file was prepared from the original file by reformatting and incorporating changes to effect uniformity in the data fields. The notes file was created at the ADC by keying the information directly to disk storage. Cross checks were performed to assure that all stars flagged as having notes have entries in the notes file and that all notes are flagged in the data file.

ID N30 running number --- DMsign DM sign --- DMzone DM zone --- DM DM number (Present for all stars) --- GC GC number (blank if not present) --- HarvaP Harvard photometric magnitude For double stars, if the position is for one component, the magnitude of that component is given and the magnitude, distance and position angle of the companion are given in the notes (remarks.dat). If the position is for the mean, center of light, or center of gravity, the combined magnitude is given and the magnitudes, distance and position angle of the components are given in the notes. Where the position is for the center of gravity, the orbital corrections used in the reduction of the observation were taken from the GC, Vol. I, Ap. II. For double stars of distances 1" to 2", there is an uncertainty as to part observed, depending upon the relative magnitudes of the components. If the components are separated and differ considerably in magnitude, then the use of screens cuts out the fainter star. There are a number of such stars and in older work the observations were reduced as the mean, or center of light. Where it seems probable that the new position is for the brighter star and the GC gives a mean, a note is given. The magnitudes of variable stars are given as a blank followed by three zeroes. 0.01mag HDSp Henry Draper (HD) spectral type Composite spectra are given as combinations; e.g. KOAO or KO+A. A few peculiar composite spectra require > 4 characters and the p's are omitted in the fields, but given in the notes. --- RAh Right ascension (equinox B1950.0) in hours Right ascension for equinox and epoch 1950.0 were brought up from epoch of observation using Newcomb's precession and the proper motions in this catalog. h RAm RA in minutes min RAs RA in seconds s RA3rd Third term in right ascension The first and second terms are not included on the original tape. 0.01s pmRA Centennial proper motion in RA 0.01s/ha v(pmRA) Centennial secular variation in pmRA 0.01s/ha mEpRA Mean epoch of RA (0.1 yr) (1900+) 0.1yr w_mEpRA weight of RA Sum of combining weights used in forming the normal position in RA. --- DE- sign --- DEd Declination (equinox 1950.0) in degrees deg DEm DEC in arcminutes arcmin DEs DEC in arcseconds arcsec DEC3rd Third term in declination 0.1arcsec pmDE Centennial proper motion in declination marcsec/a D(pmDE) Centennial secular variation in pmDE marcsec/a mEpDE Mean epoch of DEC (0.1 yr) (1900+) 0.1yr w_mEpDE weight of DEC Sum of combining weights used in forming the normal position in Dec. --- rem "*" if there is a remark in remarks.dat --- ID N30 running number --- Dot A period (.) --- rem Remark(s) --- M.C. Larkin SSDOO/ADC C.-H. Joseph Lyu Hughes STX/NASA 1996 Mar 08 The original ADC documentation by Wayne H. Warren, Jr. (1981) was used to create this ReadMe file. He also did the reformatting discussed above. UNKNOWN UNKNOWN The catalog was received on magnetic tape from the Centre de Donnees Stellaires de Strasbourg. The following modifications were made to the format in order to make the records appear more similar to the published catalog, to make them easier to read when listed, and to simplify processing to produce printed and microform versions closely approximating the published catalog in appearance: 1. Data were read and rewritten to discard leading zeroes, which make the numbers difficult to read when listed. 2. All positive Durchmusterung numbers had zeroes in the zone numbers where + signs would ordinarily be. The zeroes were changed to + signs. 3. The GC numbers and secular variations in R.A. and Dec. were changed to blank fields if not present. They were zeroes on the tape as received. 4. Several modifications were made to the spectral types: (a) Peculiar and emission symbols (p, e) were changed to lower case to conform to standard usage. (b) Composite spectra are indicated by two spectral types which run together in the 4-byte field. For types of the form K0A, a change was made to the form K0+A. (c) Peculiar HD O-star types were coded numerically; they were decoded by replacing O1 by Ob, O3 by Od, O4 by Oe5, and O0P by Oap. 5. Plus (+) signs were added to the first byte of the declination field where blanks had been previously. 6. The note indicator (byte 88) was an asterisk (*) in many cases, but for more than half of the stars having notes, a peculiar code was found which printed as b on an extended chain printer. Since there should have been no varying note characters, the latter codes were changed to asterisks for uniformity. The notes file was created and added to the machine-readable catalog. Checks were made to ensure that all records containing an * have corresponding notes and vice versa. I_80.xml 1082 I/82 SPF1 Catalogue C Anguita G Carrasco P R Loyola V N Bedin A A Naumova D D Polojentsev T A Polojentseva K N Tavastherna M S Zverev Publ. Dept. Astron., Univ. of Chile 2 181 1975 1975PDAUC...2..181A I/44 : SPF2 Catalogue (unpublished) I/78 : SPF3 Catalogue (Loyola and Shishkina, =1974PDAUC...2..159L) Fricke, W. and Ropff, A. 1963, Fourth Fundamental Katalog (FK4J, Veroeff. Astron. Rechen-Inst. Heidelberg, No. 10. Meridian observations Positional data Stars, fundamental The "First Santiago-Pulkovo Fundamental Stars Catalogue (SPF1)" contains right ascension observations of 1043 FK4 stars made during the period 1963 to 1968 with the Repsold Meridian Circle located at Cerro Calan Observatory in Chile. The FK4 stars were observed during series of observations of Southern Reference Stars (SRS) and Bright Stars (BS) international programs. Approximately 30 to 45 FK4 stars were measured during each 2- to 2-1/2-hour series, and included stars observed along the meridian between +41deg and -90deg in upper culmination and from -90deg to -68deg in lower culmination. The lower culmination observations are given in a separate table in the source reference; they are included in the file "lower". This work was made during the observations of the SRS and BS international programmes. These series of fundamental stars were periodically observed on the whole arc of meridian from +40 deg. to -68 sp deg. 211 series of observations were made with 6793 RA of stars observed. The reduction of observations was made by Zverev's quasi-absolute method (M.S.Zverev, Astr.J. USSR, 1965, v.42, p.823 and 1969, v.46, p.129.). The mean error of the positions of stars in the Catalogue is M.E. (Delta Alfa x cos Dec.) = +/- 0.008 timesec.

FK4 Number in the FK4 catalogue (Fricke and Kopff 1963). --- RAh Approximate Right Ascension 1950 (hours) h RAm Approximate Right Ascension 1950 (minutes) min DE- Approximate Declination 1950 (sign) --- DEd Approximate Declination 1950 (degrees) deg DEm Approximate Declination 1950 (minutes) arcmin dRAms(i) Correction to the FK4 right ascension in the instrumental system (RA-RA(i)) for the mean epoch of the observations. ms dRAms(FK4) Correction to the FK4 right ascension in the FR4 system for the mean epoch of the observations. ms o_dRAms(i) Number of observations for dRAms(i) --- e_dRAms(i) Mean square error of the catalogue position multiplied by cos(delta), computed with the deviations of the observations from the mean. ms Epoch Mean epoch of the observations yr Dimitri Polojentsev Pulkovo Francois Ochsenbein CDS 1995 Sep 18 Appreciation is expressed to Dr. A. Fresneau of the CDS, Strasbourg, for preparing a handwritten format description of the CDS tape at my request, and to Dr. A. Gutirrez-Moreno for sending the University of Chile publication required for comparison purposes. UNKNOWN UNKNOWN * March 1982: The SPF1 catalogue was received on magnetic tape from the Centre de Donnees Stellaires (CDS), Strasbourg. The data had been received on punched cards from the Astronomisches Rechen-Institut, Heidelberg and had been punched from a handwritten version (A. Fresneau, private communication). A check against the published catalogue (Anguita et al. 1975) revealed an extra record in the machine-readable version (FR4 #1121 with only one observation; the observation must have been removed before publication and has been deleted from the file) and one record having an incorrect FK4 number and displaced (this has been corrected), plus several stars whose right ascensions and declinations disagree by 1m or 1' between the computer file and the published catalogue (these have not been changed since the right ascensions and declinations are only approximate and are not the principal data of the catalogue). The logical record length (LRECL) of the file received (the upper and lower culmination observations were on a single file) was 88 bytes (a card image plus 8-byte allowance for CDS identification number); since bytes 50-88 were always blank, LRECL was changed to 49 bytes to save storage space. The upper and lower culmination tables were separated into two files due to the fact that lower culmination observations are made at lower altitude and are often of lower accuracy than upper culmination observations. * 18-Sep-1995: Documentation standardized at CDS. I_82.xml 1085 I/85 Cape Photographic Catalogue 2 W Nicholson M J Penston C A Murray C de Vegt Mon. Not. Roy. Astron. Soc. 208 911 1984 1984MNRAS.208..911N Positional data Proper motions Photographic catalog This catalog contains the provisional positions for 51018 stars in the Cape zone -40 deg. to -52 deg., on the FK4 system for the equinox 1950.0. The internal mean error of a single coordinate obtained from the mean of r=four plates is estimated to be less than +/- 0.1" at the mean epoch of observation, about 1962. The systematic deviation from the FK4 system in a small area is probably also about +/-0.1". New proper motions have been determined for 22731 stars which are also in the Smithsonian Astrophysical Observatory (SAO) catalogue; the formal mean error of an annual proper motion in each coordinate is about +/-0.004"/a.

The usable width of each plate is 4.1 deg. Stars were selected from the SRS and SAO catalogs, with the SRS providing the reference frame. All SAO stars were included except in crowded fields near the galactic plane, in which many SAO stars were omitted. Stars were then added by visual inspection to bring the number up to about 250, with as uniform a distribution as possible over the plate. The number of stars measured per plate varied from 70 to more than 700. The numbering system adopted is based on the South Polar Distance of a band of declination 1 deg. wide with the stars within each band being numbered sequentially in the order of right ascension. Approximate visual magnitudes have been determined from the image diameters calibrated by the V values from the published literature. Only three plates have fewer than 10 such standards; 75% of the plates have between 15 and 30. Generally, the available stars are brighter than V-9.5 mag.

ID CPC2P number --- SAO SAO number --- SRS SRS number --- RAs Right ascension seconds (1950) s DE- Sign of declination --- DEs Declination seconds (1950) arcsec mag Magnitude cmag ep Epoch of observation - 1900 a e_RAs Internal mean error in RAs arcsec e_DEs Internal mean error in DEs arcsec n_mag Magnitude status 0 = not available 1 = normal 2 = variable --- o_pos Number of plates used for position --- o_mag Number of plates used for magnitude --- del_SS Separation of SRS and CPC2 positions arcsec pmRA Annual proper motion in RA s-4/a pmDE Annual proper motion in declination marcsec/a e_pmRA Mean error of proper motion in RA s-4/a e_pmDE Mean error of pm in declination marcsec/a del_pm Larger pm diff. |CPC2-SAO| in RA or DE marcsec/a N. G. Roman ADC/SSDOO 1997 Jul 25 I_85.xml 1086A I/86A Sydney Southern Star Catalogue D S King N R Lomb J. Proc. R. Soc. N. S. W. 116 53 1983 1983 Astrometric data Positional data Proper motions This catalogue principally covers the range between -51deg. and -63.5 deg and contains positions and proper motions for 29,926 stars. 3244 faint Astrographic stars were added to supplement the stars at fainter magnitudes. Positions in standard form (hours, minutes, and seconds of time for the right ascensions and degrees, minutes, and seconds of arc for the declinations) have been added to the machine readable version of this catalogue.

The Sydney Southern Star Catalogue contains the results of the Sydney Observatory astrometric program during the two decades ending in 1983. Declination zones centered on -53.5, 58.5, -56.0, -58.5, -61.0, and -63.5 deg. have been measured and are included. The plates were taken with a 23-cm Taylor, Taylor, and Hobson camera and measured with a Grubb-Parsons photoelectric measuring machine. The reference catalogue used was the WL50. The standard error of a position based on four images is 0.10" in either coordinate. A 2.3 magnitude diffraction grating was used to produce side images shifted from the central image in declination. The stars selected were compiled from the Cape Photographic Catalogue for 1950 (CPC) (Jackson and Stoy 1954-1958), International Reference Stars (IRS) (Scott 1962), Cape Zone Cataloge for 1900 (ZC) (Gill and Hough 1923, Spencer Jones and Jackson 1936), Albany General Catalogue (GC) (Boss 1937) and the Sydney Astrographic Catalogue (AC) (Nangle and Wood 1925-1971). The Sydney AC was used to obtain 3244 supplementary faint stars so that about one star per square degree is in the photographic magnitude range 11.0 to 11.5. All of the AC stars were given a magnitude of 12.0 to distinguish them as AC stars although they are presumed to be in the stated photographic magnitude range. In the area south of -63.5 deg., only the IRS stars were selected for measurement. This was to give complete plate coverage for the determination of plate constants for the plates centered at -6358.5 deg. 395 IRS stars are included in this zone. CPC stars and AC stars were selected for measurement between declinations -52deg. and -63.5 deg. Between -51deg. and -52deg., the measuring list was prepared by supplementing the few CPC stars in this area with ZC stars, GC stars, and IRS stars. In general, stars brighter than photographic magnitude 6.0 were excluded and stars brighter than photographic magnitude 8.1 had their first order side images measured as well as the central image, giving three measurements.

num Number --- magpg Photographic magnitude 0.01mag RAh Hours right ascension (1950) h RAm Minutes right ascension (1950) min RAs Seconds right ascension (1950) s DE- Sign of declination --- DEd Degrees declination (1950) deg DEm Minutes declination (1950) arcmin DEs Seconds declination (1950) arcsec RAsec Right ascension in seconds 0.001s DEsec Declination in arcseconds 0.01arcsec Epoch Epoch - 1900.000 0.001yr N No. observations --- pmRA Proper motion in right ascen. 0.0001s/yr pmDE Proper motion in declination 0.001arcsec/yr num Number --- magpg Photographic magnitude 0.01mag RAh Hours right ascension (1950) The positions are for the equinox B1950 and the reference system used was Washington El Leoncito 50. h RAm Minutes right ascension (1950) min RAs Seconds right ascension (1950) s DE- Sign of declination --- DEd Degrees declination (1950) deg DEm Minutes declination (1950) arcmin DEs Seconds declination (1950) arcsec RAsec Right ascension in seconds 0.001s DEsec Declination in arcseconds 0.01arcsec Epoch Epoch - 1900.000 0.001yr N No. observations --- Nancy G. Roman SSDOO/ADC 1995 Mar 28 We thank Dr. Lomb for supplying us with the machine-readable version of the Sydney Southern Star Catalogue and for a preprint of the Source Reference. UNKNOWN UNKNOWN Construction of the current version of the Sydney Southern Star Catalogue The machine-readable file was received on magnetic tape from Dr. N. R. Lomb of the Sydney Observatory in November, 1983 in excellent shape. As received, the catalogue contained two files. The primary catalogue file contained right ascensions and declinations in milliseconds of time and hundreths of a second of arc, respectively. The second file contained the data for both the faint Astrographic stars and the southern IRS stars. In the present version, sexigesimal positions (hours and degrees) have been added in addition to the form given on the tape as received and the Astrographic and IRS data have been divided into separate files. I_86A.xml 1087B I/87B LHS Catalogue, 2nd Edition W J Luyten University of Minnesota, Minneapolis, September ??? ??? 1979 1979 I/98 : NLTT Catalogue (proper motion exceeding 0.2" annually) Proper motions The catalogue gathers stars with large proper motions, the large majority coming out of the Bruce Proper Motion Survey (W.J. Luyten). 804 fields in the Palomar Survey have been hand-blinked or processed by an automated blink-machine; 160 low galactic latitude fields could not be handled. There are therefore many less stars with high proper motion south of -33 degrees (limit of the Palomar Survey) compared to the Northern hemisphere. Stars with proper motions larger than 2arcsec/yr are numbered 1 to 100; stars with proper motions between 1 and 2arcsec/yr are numbered 101 to 1000 ; numbers 1001 through 5000 are assigned to stars with proper motions between 0.5 and 1arcsec/yr. The stars which appear to have motions between 0.480 and 0.499arcsec/yr have been assigned numbers larger than 5000. Numbers larger than 6000 refer to Appendix II of the printed publication, containing stars for which at one time or another a value larger than 0.49arcsec/yr was published; these numbers are not listed in the printed version of the catalogue. All proper motions have been reduced to the Palomar-Bruce system. The catalogue supersedes the "Catalogue of Stars with Motions exceeding 0.5" annually" (LFT) published in 1955 (CDS ref. <I/54>)

LHS designation --- Note '*' note detailed in file "notes.dat" --- Name Other designation --- RAh Right Ascension 2000 (hours) h RAm Right Ascension 2000 (minutes) min RAs Right Ascension 2000 (seconds) s DE- Declination 2000 (sign) --- DEd Declination 2000 (degrees) deg DEdm Declination 2000 (deci-minutes) 0.1arcmin RA1950h Right Ascension 1950 (hours) h RA1950m Right Ascension 1950 (minutes) min RA1950s Right Ascension 1950 (seconds) s DE1950- Declination 1950 (sign) --- DE1950d Declination 1950 (degrees) deg DE1950dm Declination 1950 (deci-minutes) 0.1arcmin Rmag Red magnitude mag Pmag Photographic magnitude mag l_Pmag '+' when Pmag is a lower value --- Sp Spectral type --- Color classification based on colour --- pm Total proper motion number=1 the proper motion is empty for LHS 6219, indicated as "plate flaw" in the catalogue. arcsec/yr u_pm Uncertainty flag on proper motion --- pmPA Position angle of proper motion number=1 the proper motion is empty for LHS 6219, indicated as "plate flaw" in the catalogue. deg Disc Original (discovery) name or author --- LHS Star --- Text Text of note --- Francois Ochsenbein CDS 1998 Jul 15 UNKNOWN UNKNOWN * March 1984: first announced in CDS Inf. Bull. 26 * 16-Mar-1995 (version 'A'): reformatted at CDS, transformed to lower-case, and added notes.dat. Duplicate entry LHS 3224 has been deleted Erroneous BD+04 3561 number for Barnard's star (LHS 57) removed * 15-Jul-1998 (version 'B'): following a message by John Gizis (gizis@stratford.phast.umass.edu), two erroneous records (LHS 2297 and 3038) have been corrected. I_87B.xml 1090 I/90 Positions of 502 Stars in Pleiades Region H Eichhorn W D Googe C F Lukac J K Murphy MmRAS 73 125 1970 1970MmRAS..73..125E I/163 : U.S. Naval Observatory Pleiades Catalog (Van Flandern 1969) Binnendijk L. 1946, Ann. Sterrew. Leiden, 19, 2 Dieckvoss W. & Kox H. 1955, Astr. Nachr., 282, 217 Eichhorn H. 1960, Astr. Nachr., 285, 233 Eichhorn H. 1970, The Behaviour of Magnitude Dependent Systematic Errors. Paper pres. to Conf. of Phot. Astr. Technique at Tampa FL. Eichhorn H., Googe W. & Gatewood G. 1967, Astr. J., 72, 626 Eichhorn H. & Gatewood G. 1967, Astr. J. 72, 1191 Eichhorn H., Googe W., Lukac C. & Murphy J.K. 1969, USATOPOCOM Tech. Report No. 70 Eichhorn H. & Williams C.A. 1963, Astr. J., 68, 221 Googe W. 1967, Astr. J., 72, 620 Hertzprung E. 1947, Ann. Sterrew. Leiden, 19, 1A Koenig A. 1924, Astron. Nachr., 222, 177 Lacroute P. 1964, Ann. Obs. Strasbourg, 6 Lukac C. 1967, Astr. J., 72, 620 Positional data Proper motions Regional catalog The catalog contains the right ascensions and declinations (equinox B1900.0 and epoch B1955.0) of 502 stars in a region of about 1.5 degrees square in the Pleiades cluster, centered on Eta Tau. These coordinates have been derived from measurements of stellar images obtained with 65 exposures of various durations on 14 photographic plates with two telescopes at McCormick Observatory and Van Vleck Observatory. The plates were reduced by the plate overlap method, which resulted in a high degree of systematic accuracy in the final positions. Data in the machine version include Hertzsprung number, color index, photovisual magnitude, right ascension and declination and their standard errors, proper motion, and differences between the present position and those of Koenig (1924). Data for exposures, plates, and images measured, present in the published catalog, are not included in the machine version.

HID Hertzsprung Number 1947 Ann. Sterrew. Leiden, 19, 1A --- B-V Color Index mag mag Photovisual Magnitude mag RAh Right Ascension 1955 hours h RAm Right Ascension 1955 minutes min RAs Right Ascension 1955 seconds s e_RAs Standard Error in Right Ascension s DEd Declination 1955 degrees deg DEm Declination 1955 arcmin arcmin DEs Declination 1955 arcsec arcsec e_DEs Standard Error in Declination arcsec RMSRA RMS for Right Ascension A large RMS indicates that the individual measurements that contribute to a listed coordinate of a certain star show an agreement worse than that expected on the basis of the weighting of the individual measurements; and a small RMS indicates that the positions from the individual measurements of a star agree better than expected. The product 'standard error times RMS' is then a good approximation of the dispersion of the individual contributing positions around their published mean, although not this dispersion itself. --- RMSDE RMS for Declination --- pmRA Proper Motion in Right Ascension Since all positions involved refer to the orientation of the coordinate system at 1900.0, the proper motion components also are valid for 1900.0. Since Konig gives the standard error of his positions as 0.065", and the typical standard error of the reference star's position from this investigation is around 0.03", 0.002" is obtained as the standard error of a proper motion component. This is comparable to, but typically better than the accuracy of Hertzsprung's proper motions. arcsec/ka pmDE Proper Motion in Declination arcsec/ka dpmRA Difference in Proper Motion RA Proper motion in right ascension difference between Hertzsprung's and present work arcsec/ka dpmDE Difference in Proper Motion Dec Proper motion in declination difference between Hertzsprung's and present work arcsec/ka dRA Difference in RA Difference in right ascension between Koenig's and present work positions (1924 Astr. Nachr., 222, 177) carcsec dDE Difference in Dec Difference in declination between Koenig's and present work positions carcsec Julie Anne Watko SSDOO/ADC 1996 Feb 21 I_90.xml 1092 I/92 Yale Zone Catalogue -60 to -70 F W Fallon Yale Trans. 32, part II ??? ??? 1983 1983TOYal..322...1F Astrometric data Proper motions Positional data The original plans for the Southern Yale Zone catalogs were to reobserve and derive strengthened positions and proper motions for all stars in the zones -30 deg to -50 deg and -60 deg to -90 deg. Having been delayed by an incredible number of misfortunes, the zone -60 deg to -70 deg has now been published (Fallon 1983). The catalog contains the measured positions and derived proper motions for the stars in this zone. In addition to the data in the published catalog, this file lists the numbers of the plates measured for each star.

Number Serial number. --- CPD Designation in the Cape Photographic Durchmusterung (CPD, Gill and Kapteyn 1896). --- RAh Right Ascension for Equinox 1950 (hours) h RAm Right Ascension 1950 (minutes) min RAs Right Ascension 1950 (seconds) s DE- Declination for Equinox 1950 (sign) --- DEd Declination 1950 (degrees) deg DEm Declination 1950 (minutes) arcmin DEs Declination 1950 (seconds) arcsec Epoch Epoch for position. yr pmRAs Annual proper motion in RA s/yr pmRA Annual proper motion in RA (*cos(delta)) arcsec/yr pmDE Annual proper motion in DE arcsec/yr Mag Visual magnitude. mag n_Mag An asterisk indicates constructed magnitude. See note in "adc.doc". Note however that the following stars have very high magnitudes are variables or very late-type stars: Magnitude 19.0 for stars #1707 6181 7370 7883 8852 10606 11237 12261 12614 13157 13236 13868 Magnitude 18.8 for stars #2091 5092 --- CI Color index. mag Images Number of images measured. A pair of grating images is counted as one image. --- Plates Number of plates measured. --- PlateList 18 two-digit numbers identifying plates on which images were measured. If the number measured is less than 18, a zero fill is used for blank fields. --- FieldCode Field star code. This code is always zero, meaning a standard reduction from at least two overlapping plates. See also note in "adc.doc". --- pmCode Proper motion code. See detailed note in "adc.doc". Short explanations: A = Proper motion taken directly from the CPC (therefore on FK3 system). B = Proper motion Yale - LaPlata positions. C = Same as B but mean from overlapping LaPlate positions D = LaPlata position from NFK (Peters 1907) E = Proper motion from Sydney - Yale plates F = Proper motion from mean of Yale/Sydney compared with LaPlata. G = not explained code; exists for stars #13513 13578 13684 13765 13791 #13814 14256 14257 14271 14299 14384 14411 14432 14470 14496 14497 H = not explained code; exists for star #13661 --- adc.doc Document file by Nancy G. Roman and Wayne H. Warren Jr. Francois Ochsenbein CDS 1994 Jul 20 UNKNOWN UNKNOWN Document editing: Nancy G. Roman [SSDOO/ADC] added the key words and description and modified the format table slightly to correspond with the current standard document on 20-Feb-1995. I_92.xml 1096 I/96 Astrographic Catalogue, +01 to +31 Degrees A Fresneau Astron. Journ. 88 1378 1983 1983AJ.....88.1378F Astrographic zones Positional data Magnitudes, photographic This machine-readable version of the Astrographic Catalogue (AC), zones +01 to +31 degrees is the result of the determination of mean values for position and magnitude at a mean epoch of observation for each unique star in the original catalogs. The zones considered here (Oxford, Paris, Bordeaux, Toulouse, Algiers [partial]) contained 1,870,976 individual measures, from which the catalog of mean data for 1,025,208 stars was derived. Further analysis by Dr. D.W. Dunham and at the ADC yielded an additional 27897 apparently duplicate entries, which were eliminated to produce the final catalog. The estimated mean standard errors for positional and magnitude data are 0.4 arcsec in each coordinate and 0.4 mag, respectively. Data in this version include <m(pg)>, <Epoch>, <RA> at mean epoch, <DEC> at mean epoch. The mean values are unweighted. No star identifications are provided; hence the user must select stars from the catalog and then identify them in other catalogs or on charts using the equatorial coordinates.

RA Right ascension at mean epoch given (1950.0) deg DEC Declination at mean epoch given (1950.0) deg Mphoto Mean photographic magnitude. mag MeanEp Mean epoch of all observations for this star unweighted mean epoch yr M.C. Larkin SSDOO/ADC C.-H. Joseph Lyu Hughes STX/NASA 1996 Mar 08 Appreciation is expressed to A. Fresneau for making the machine-readable catalog available for distribution from the ADC and for reviewing and commenting on a preliminary version of this document. L. H. Wasserman and D. W. Dunham kindly transmitted their findings back to the ADC, and Dr. Dunham supplied his program for elimination of duplicate entries and a copy of his modified version, formatted specifically for ADC purposes. The combined efforts of these colleagues have produced an improved version of the machine catalog for distribution to the astronomical community. The original ADC documentation by Wayne H. Warren, Jr. (1983) was used to create this ReadMe file. Dr. Warren was also responsible for the preparation of the catalog for archiving as described above. UNKNOWN UNKNOWN The machine-readable AC Survey +01 deg to +31 deg was prepared from a tape supplied by the author (A. Fresneau) during a visit to the Astronomical Data Center (ADC) on 21 July 1983. As received, the file was found immediately to contain some stars at various right ascensions which were apparently appended to the file; however, a copy of the unsorted file was supplied to R. L. Millis of Lowell Observatory, where he and L. H. Wasserman found additional groups of stars out of RA order. The arrangement of the data was a result of the reduction procedure (Fresneau 1983c) and should not have been unexpected. Since the stars should be in some kind of rigorous order for data searching purposes, the file was sorted by increasing RA with decreasing DEC as the secondary sort field and increasing magnitude as the tertiary sort field. A copy of the sorted file was then supplied to D. W. Dunham, who discovered 19873 records where all data were identical and 8024 records where differences were too small to be accounted for by duplicity at AC resolution. A separation criterion of 0.00031 deg was used to eliminate all stars whose positions matched to within the limit in both RA and DEC. Since Dunham also changed some of the faint magnitudes to suit his own applications, only his program to eliminate duplicates was used to process the original sorted version to produce the present file with no magnitude modifications and the revised format. Although a more detailed analysis may be performed later, Dr. Warren concurs with the present method and production of this file for distribution until such time as improved criteria may be established. It is important to note and consider the fact that there are quite a few stars present having magnitudes in the 16-18 range and others for which punching errors have occurred, resulting in magnitudes such as 79.3, 79.5, 26.0, 75.3, 49.5, etc. (77 stars fainter than 16 magnitude, including definite punching errors). These errors have not been corrected in the present machine version. I_96.xml 1097 I/97 Perth 75 Catalogue I Nikoloff E Hog Bickley W. Australia, Perth Observatory ??? ??? 1982 1981QB881.N55...... I/62 : The Perth 70 Catalogue of Positions of 24900 Stars (Hog+ 1976) I/143 : FK4 Catalogue (Fricke & Kopff, 1963) I/149 : FK5 Catalogue, part I : Basic Fundamental Stars (Fricke et al. 1988) I/175 : FK5 Catalogue, part II: Extension) (Fricke et al. 1991) Fricke, W., and Kopff, A. 1963, Veroeff. Astron. Rechen-Inst. Heidelb., Nos. 10, 11 (CDS Catalogues <I/143>) Positional data Proper motions Meridian observations Stars, fundamental The catalog contains results of approximately 60000 photoelectric meridian circle observations made at the Perth Observatory for 1156 FK4 and 1433 FK4 Supplement stars south of declination +38 degrees. The catalog reports proper motions and positions at epoch and equinox B1950.0. The data used to derive the epoch 1950 positions are included in the catalog so that originally observed positions may be recomputed and used for geodetic purposes until the FK5 becomes available. The mean error of an individual position in this catalog is 0.07" in right ascension and 0.13" in declination at a zenith distance of 45 degrees, while the mean error of the PERTH 75 system is 0.05" in right ascension and 0.10" in declination. The positions do not contain the large systematic errors of the FK4 (Fricke and Kopff 1963), which can be, for example 0.3" in right ascension for declination < -75 degrees. Data in the catalog included FK4 (FK4S) number, observed visual magnitude, spectral type used for computing refraction, right ascension and declination (equinox and epoch B1950.0), annual proper motion, observed residuals, numbers of accepted observations, and code to indicate if parallax and/or radial velocity has been used in computing apparent positions.

FK4 Star number in FK4 (< 2000) or FK4S (> 2000). --- Vmag Observed or FK4 visual magnitude (see n_Vmag) mag n_Vmag An "s" (lower case) if Vmag has been taken from the FK4. --- Sp The HD spectral type --- RAh Right Ascension B1950 (hours) right ascension and declinations at Epoch=B1950.0, referred to equator and Equinox=B1950.0. The determination of the equator and zero point in R.A. was made from observations of approximately 40 FK4 stars per night. h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec pmRA Annual proper motion in R.A. s/yr pmDE Annual proper motion in Dec. arcsec/yr O-C(RA) Observed residual in apparent RA cos(Dec), in the sense Observed minus FK4 or FK4S. 10mas O-C(DE) Observed residual in apparent in Dec., in the sense Observed minus FK4 or FK4S. 10mas o_RAs Number of accepted observations in R.A. --- o_DEs Number of accepted observations in Dec. --- EpRA-1900 Epoch - 1900 for the observation in R.A. yr pFlag A letter "p" (lower case) if parallax and/or radial velocity used in computing apparent positions. --- F. Ochsenbein CDS 1996 Nov 28 This document is just an adaptation of the "Documentation for the machine-readable version of the Perth 75 catalogue" written by Wayne H. Warren Jr. in February 1984. I_97.xml 1098A I/98A NLTT Catalogue W J Luyten Minneapolis, University of Minnesota ??? ??? 1979 1979 W J Luyten H S Hughes Proper Motion Survey with the Forty-Eight inch Schmidt Telescope LV ??? ??? 1980 1980LP.....55....1L Proper motions The NLTT catalog is a collection of stars with proper motions exceeding 0.18"/yr found by Luyten and his coworkers. The First Supplement to the NLTT catalog is the result of continued plate analysis and contains data for 398 stars with proper motions greater than 0.179"/yr. A number of corrections to the data in the published catalog have been entered in the machine-readable version, including the omission of duplicate entries and those stars later determined to show no motion. The catalog contains, in addition to the proper motions, 1950 equatorial coordinates, a flag indicating the approximate accuracy of the positions, estimated red and photographic magnitudes, spectral types, and flags indicating a change from the published volume and the presence of the star in the supplement.

Name Star designation number=1 Identifiers without prefixes are DM (Bonner and Cordoba Durchmusterungen, written with a colon), or Luyten numbers from the Bruce Proper Motion Survey (L numbers) or the Luyten-Palomar Survey (LP numbers), the former in zones -45 to -89 deg and the latter in zones +89 to -44 deg. Other miscellaneous identifiers (Oxf = Oxford AC, Grw = Greenwich AC; U = Upgren; R = Ross, etc...). An asterisk (*) in the identification field indicates that a not exists in the "notes" file of the catalog. --- RAh Hours RA, equinox B1950.0 h RAm Minutes RA, equinox B1950.0 min RAs Seconds RA, equinox B1950.0 s RAm2 Right ascension, equinox B1950.0, minutes only min n_RAs Flag on RA: 1 = RA originally reported in 0.1min --- DE- Sign Dec, equinox B1950.0 --- DEd Degrees Dec, equinox B1950.0 deg DEm Minutes Dec, equinox B1950.0 arcmin Rmag Estimated red magnitude mag n_Rmag Flag on Rmag number=2 ':' indicates a larger uncertainty '+' indicates a mag fainter than reported value 'v' indicates a known variability --- Ptg Estimated photographic magnitude mag n_Ptg '+' Flag on Ptg number=2 ':' indicates a larger uncertainty '+' indicates a mag fainter than reported value 'v' indicates a known variability --- SpType Spectral type; lowercase letters represent estimated color classes or ranges. --- pm Relative proper motion, equinox B1950.0 number=3 The total proper motion is reported. The RA/DE proper motions can be computed with the formulae pmRA = pm.sin(pmPA) pmDE = pm.cos(pmPA) arcsec/yr u_pm ':' if proper motion is uncertain --- pmPA Position angle of PM vector number=3 The total proper motion is reported. The RA/DE proper motions can be computed with the formulae pmRA = pm.sin(pmPA) pmDE = pm.cos(pmPA) deg u_pmPA ':' if position angle is uncertain --- ModFlag 'A' indicates data have been changed (see Appendix A of adc.doc or adc.tex) --- SupplFlag '1' indicates a star from First Supplement (Luyten and Hughes, 1980) --- Name Star designation in one of many catalogs --- RAh Hours RA, equinox B1950.0 h RAm Minutes RA, equinox B1950.0 min RAs Seconds RA, equinox B1950.0 s DE- Sign Dec, equinox B1950.0 --- DEd Degrees Dec, equinox B1950.0 deg DEm Minutes Dec, equinox B1950.0 arcmin Text Note for star in free-form text --- adc.doc Documentation by Warren et al. (ascii) doc.tex Documentation by Warren et al. (LaTeX) Francois Ochsenbein CDS 1995 Jun 27 UNKNOWN UNKNOWN * A large number of corrections were performed at ADC, see section 3 of "adc.doc" or "doc.tex" files * From the "Selected Astronomical Catalogs" Vol. 1 CD-ROM (1992), directory /astrom/nltt * 30-Jun-1995: bad decimal point (blank or dashed) corrected in records 9694 (LP 198-153), column DEm 37692 (LP 381- 80), column pm 38236 (CD-68:1403), column Rmag 52719 (LP 983- 71), column DEm I_98A.xml 1099 I/99 Brorfelde Meridian Catalogues 1964-1976 S Laustsen Publ. Mindre Medd. Kbh. Obs. No. 197 ??? ??? 1968 1973A&AS....9....1F H J Fogh Olsen Astron. Astrophys. Suppl. 9 1 1973 1973A&AS....9....1F H J Fogh Olsen V Helmer Astron. Astrophys. Suppl. 30 349 1977 1977A&AS...30..349O V Helmer H J Fogh Olsen Astron. Astrophys. Suppl. 49 13 1982 1982A&AS...49...13H L Helmer C Fabricius O H Einicke C Thoburn Astron. Astrophys. Suppl. 53 223 1983 1983A&AS...53..223H L Helmer C Fabricius O H Einicke C Thoburn L V Morrison Astron. Astrophys. Suppl. 55 87 1984 1984A&AS...55...87H Positional data Meridian observations This catalog contains positions and magnitudes for 1577 stars with visual magnitudes brighter than 11.0. The observations were made with the 7-inch transit circle at the Copenhagen University Observatory from July 1981 to May 1982. The positions are reduced to the FK4 system for each night and over the whole meridian. The mean errors of the catalog entries are: in right ascension 0.006 seconds/cos(declination); in declination, 0.10"; and in magnitude, 0.06mag. The catalog contains 425 FK4 stars used for the adjustment to the FK4; 167 stars from the AGK3 zones +88deg. and +89deg.; 115 stars from the zone around the North Galactic Pole; stars from several PZT zones; some faint GC stars; reference stars for radio fields; and a few stars from earlier Brorfelde programs. The internal errors of a single observation are for right ascension, 0.0138 seconds/cos(delta), for declination, 0.216", and for the magnitude, 0.132 mag.

ID Internal number --- BDsign BD zone sign --- BDzone BD zone --- BDnum BD number within zone --- BDsuf BD suffix --- AGK3sign AGK3 zone sign --- AGK3zone AGK3 zone --- AGK3num AGK3 number within zone --- AGK3suf AGK3 suffix --- FK4 FK4 or NPZT number For FK4 no other reference is given. --- GC GC number --- mag Approximate visual magnitude 10-2mag Sp Spectral Type --- RAh Right Ascension (1950.0) hours h RAm Right Ascension (1950.0) minutes min RAs Right Ascension (1950.0) seconds s o_RAs Number of observations in Right Ascension --- EpRA Epoch - 1900 for RA a plxRA Parallax factor in RA * 100 --- DE- Declination (1950.0) sign --- DEd Declination (1950.0) degrees deg DEm Declination (1950.0) arcminutes arcmin DEs Declination (1950.0) arcseconds arcsec o_DEs Number of observations in Declination --- EpDE Epoch - 1900 for Dec a plxDE Parallax factor in Dec * 100 --- ADS ADS or BDS number 0 = neither ADS nor BDS number given AY = ABC AX = A' --- cat Catalogue identification 001 = Helmer et al. =1983A&AS...53..223H 002 = Helmer at al. =1994A&AS...55...87H program stars 003 = Ibid. FK4 stars (no cross references are given) --- ID1 Identification number within catalogue --- ID2 Internal identification --- RAh Right Ascension (1950.0) hours h RAm Right Ascension (1950.0) minutes min RAs Right Ascension (1950.0) seconds s o_RAs Number of observations in RA --- EpRA Epoch of observation for RA a DE- Declination (1950.0) sign --- DEd Declination (1950.0) degrees deg DEm Declination (1950.0) arcminutes arcmin DEs Declination (1950.0) arcseconds arcsec o_DEs Number of observations in Dec --- EpDE Epoch of observations in Dec a mag Observed magnitude mag o_mag Number of observations in mag --- Sp Spectral type --- DMsign Durchmusterung zone sign --- DMzone Durchmusterung zone --- DMnum Durchmusterung number within zone --- DMsuf Durchmusterung suffix --- AGK3sign AGK3 zone sign --- AGK3zone AGK3 zone --- AGK3num AGK3 number within zone --- SAOC SAOC number --- HD HD number --- GC GC number --- FK4 FK4 or FK4 Sup number --- n_FK4 * = program star --- Gleise Gleise number --- ADS ADS number --- ADSsuf ADS suffix --- ignore Asterisk --- Julie Anne Watko SSDOO/ADC 1996 May 07 I_99.xml 1108 I/108 Cape Photographic Durchmusterung D Gill J C Kapteyn Cape Photographic Durchmusterung, Ann. Cape Obs. 3 ??? ??? 1895 1896AnCap...3....1G D Gill J C Kapteyn Cape Photographic Durchmusterung, Ann. Cape Obs. 4 ??? ??? 1897 1897AnCap...4....1G D Gill J C Kapteyn Cape Photographic Durchmusterung, Ann. Cape Obs. 5 ??? ??? 1900 1900AnCap...5....1G Surveys Durchmusterungen The "Cape Photographic Durchmusterung" (CPD, Gill and Kapteyn 1895-1900) is a photographic survey of southern stars in the declination range -18 deg to -90 degrees. The original goal of the work was to carry out a southern survey similar to those of the "Bonner Durchmusterung" (BD, Argelander 1859-1862, see also Kuestner 1903) and Schoenfeld (1886) and the "Cordoba Durchmusterung" (CD, Thome 1892-1932) but using photographic plates which would provide a permanent record of the sky at the epoch of observation. The summary of the positional uncertainties quoted in the third volume of the published catalog gives +/- 0.28 sec (R.A.), +/- 0.044 arcmin (Dec.) for zones -18 to -57 degrees, +/- 0.157 sec + 0.0764/cos(delta) sec (R.A.), +/- 0.056 arcmin (Dec.) for zones -58 to -85 degrees, and +/- 0.157 sec + 0.0353/cos(delta) sec (R.A.), +/- 0.0127 arcmin (Dec.) for the polar plate where, as explained in the intro- duction to the third volume, many positions were derived from rectangular coordinates (these are positions reported to 0.1 sec (R.A.) and 0.001 arcmin (Dec.) in the -86 to -89 degree zones in the catalog). The probable error of a photographic magnitude, as determined by combining results for different magnitudes and weighting proportionately according to the numbers of stars in each class of magnitude, is given as +/- 0.055 mag. From an analysis of the faint magnitude limits on the plates discussed in the third volume introduction, the catalog as a whole can be considered complete to photographic magnitude 9.2, but it is stated that it will be found practically complete, in or near the Milky Way, to magnitude 9.5.

The complete catalog is contained in the data file, and corrections published in all errata have been made to the data. The machine version contains 454877 records, but only 454875 stars (two stars were later deleted, but their logical records are retained in the file so that the zone counts are not different from the published catalog). A list of corrections made to the original data as a result of errata published in the three volumes is presented in cpchg.dat. No other corrections or changes have been incorporated into the original data, e.g., from more modern positions and magnitudes or comparison with other catalogs. The original ADC document contains the total number of stars in each declination zone and the number added and deleted in each zone. Data are present for all stars in the catalog, including some which have been deleted in the errata; these have been flagged by a "D" in byte 11 of each respective record, but the records and data have been left in the machine version in order not to change the star counts and numerical sequencing and so that the stars appear in the correct locations if the catalog is sorted by right ascension.

cat The catalog prefix --- zonesign The sign of the declination zone --- zone The declination zone deg num The number of the star within the zone --- suppl star in corrigenda a, b, or c: star is added in the corrigenda; D: star is deleted in the corrigenda --- mag Estimated photographic magnitude 20.0 = neb; 30.0 = var mag RAh Hours of right ascension, 1875 h RAm Minutes of right ascension, 1875 min RAs Seconds of right ascension, 1875 precision varies; tenths can be blank s DE- Sign of declination --- DEd Degree of declination, 1875 deg DEm Minutes of declination, 1875 Only bytes 27-30 are used in zones north of -86 deg; the complete field is used for many stars on the polar plate. arcmin zonesign The sign of the CP zone --- zone The CP zone --- num The CP number --- n_num Note on star number --- field The field changed --- old The printed value --- new The corrected value --- note Comments --- adc.doc The original ADC document Nancy G. Roman NSSDC/ADC 1994 Nov 12 This project owes its completion to the extensive work and striving for perfection of Barry Rappaport, who supervised the punching of all data, ran numerous machine and manual checks on completed zones, and prepared the preliminary tape of the finished catalog. The quality work of the keypunchers at Case Western Reserve University and Syntronix, Sherman Oaks, California is also greatly appreciated. The encouragement and support of the NSSDC Director, James I. Vette, made the completion of this project possible. This document is based on the original ADC document prepared by Wayne H. Warren, Jr. UNKNOWN UNKNOWN The data in the machine-readable "Cape Photographic Durchmusterung" were keypunched directly from the published catalogs. The northern zones (-18 to -32 degrees and -35 degrees) were punched at Case Western Reserve University under the direction of B. N. Rappaport, who initiated the work and used the data as part of a project on the production of star charts by computer. However, only zones -18 through -26 degrees and -28 degrees had been verified and checked thoroughly, and some zones had not been completed. Mr. Rappaport was contacted and volunteered to continue the project and to oversee the punching and verifying of the remaining zones and those not verified and checked at Case. These zones were processed by a commercial firm with funding provided by the National Space Science Data Center, but all systematic checking of the completed zones was carried out by Mr. Rappaport on a volunteer basis. The zones were rechecked for counts and errata corrections, and the data reformatted to the standard DM catalog structure at the ADC by the author. The individual zones were then concatenated from disk data sets to a single magnetic tape file in CPD number order from north to south. Users should note that, due to corrections inserted from the errata, the CPD stars are not strictly in right ascension order within each zone; hence, if the catalog is sorted by right ascension, e.g., for search purposes, some CPD numbers will become disordered. I_108.xml 1110 I/110 Occultation Double-Star Observations D S Evans IAU Colloquium No. 62, Current Techniques in Double and Multiple Star Research, Lowell Obs. Bull. 167, p. 73 ??? ??? 1983 1983LowOB.167...73E Stars, double and multiple Occultations This catalog contains data on 224 double stars observed photoelectrically during lunar occultations. The author cites the advantages of this method of double star detection as increased resolution, accuracy of the vector separations of roughly one-half arcsecond or better, and the opportunity to make photometric determinations of the magnitude differences between components. The vector separation is the true separation projected along a line perpendicular to the actual lunar limb. The catalog is a compilation of twelve years of observations from the literature (through roughly 1980). It is divided into three files. The first file, data1.dat, contains information on stars brighter than visual magnitude 6.7. The second, data2.dat, lists SAO catalog stars fainter than magnitude 6.7. The third file, data3.dat, contains data on faint stars with no SAO number. For these stars, data on their magnitudes or spectral types may be absent. In many cases there are multiple records per star, reflecting separate observations. The records are arranged by SAO number or other identifier, and contain visual magnitudes, spectral type, observing run number, a subjective grade of the probability of being double, the vector separation with computed error, position angle, and the lunar limb slope and its error. It also includes the magnitude difference between the components in (somewhat arbitrarily assigned) blue and red band passes. In the case of a triple star, the run number is repeated and the data for the triple given with magnitude differences from the brightest star.

SAO SAO Number --- NAME Other Name for Star --- MAG Magnitude mag Sp Spectral Type --- RUN Run Number of the Observation Sources McDonald Observations: M100-1871: Astron. J. 76, 1109, 1971: M1875-M1893, M2102-M22221, M2304-2711: Astron. J. 78, 482, 1973: M1902-M2020, M2250-2262: Astron. J. 80, 449, 1975: M2713-M3712: Astron. J. 80, 689, 1975: M3713-M4009: Astron. J. 81, 650, 1976: M4010-M4245, Astron. J. 82, 631, 1977 (but M4045, M4058, M4059, M4148, Astron. J. 82, 640, 1977): M36/7, M36/8, M4247-M4729: Astron. J. 83, 1100, 1978: M4730-M5222, Astron. J. 85, 478, 1980 (but M5100-M5112: Astron. J. 85, 490, 1980), and M5223-M5646, Astron. J., submitted. Geneva Observations: G12-G38: Astron. J. 80, 445, 1975. Tonantzintla Observations: T001-023: Astron. J. 79, 1299, 1974. Iowa Observations: EB002, EB021: Astron. J. 76, 1131, 1971: EB001-EB121, Astrophys. J. Supp. Ser. 28, 405, 1974: EB122-EB320, : Astrophys. J. Supp. Ser., 34, 493, 1977: EB321-562: Astrophys. J. Supp. Ser., 40, 475, 1979: EB585-592: Astrophys. J. Lett. 228, Llll, 1979. Hamburg Observations: All H numbers, Astron. Astrophys., 48, 245, 1976. Victoria Observations: Vl-V2: Publ. Dom. Astrophys. Obs. 14, 271, 1974: Vl-V32, J. Roy. Astron. Soc. Canada, 72, 305, 1978. Illinois Observations:-I7701-I7865: Astron. J. 85, 1053, 1980. Flagstaff Observations: F, Astron. J. 84, 872, 1979 and private communications. Peterson et al.: P: Astron. J. 86, 280, 1981. Special Stars: Beta Scorpii: Astron. J. 82, 414, 1977. Astron. J. 82, 495, 1977, Astron. J. 83, 438, 1978: Astron. J. 84, 257, 1979. Sigma Scorpii: Publ. Astron. Soc. Pac. 86, 116, 1974. Beta Capricorni: Astrophys. J. 228, 497, 1979. --- DAY Observation Date Day --- MONTH Observation Date Month --- YEAR Observation Date Year --- G Grade 0 No Duplicity 1 Possible Duplicity 2 Probable Duplicity 3 Certain Duplicity Grades are based on statements by observers. --- n_G Remark on G Asterisks (*) denote places where corrections have been applied to published figures, whether errors of star numbers or run numbers in original records or notes. Most commonly corrections have been made as far as can be deduced from the original sources, to bring the column of position angle values to those appropriate to position angles from the brighter to the fainter component. Most changes have been made by 180 degrees. --- SEP Vector Separation marcsec e_SEP Computed Error of Vector Separation marcsec n_SEP Remark on SEP (see note on n_G) --- PA Position Angle Position Angle on the lunar limb as modified by the slope deduced in favorable cases from the spacing of the diffraction bands on the occultation trace. deg n_PA Remark on PA (see note on n_G) --- SL Limb Slope --- n_SL Remark on SL (see note on n_G) --- e_SL Error of SL --- dB Blue Differential Magnitude mag e_dB Error of dB mag n_dB Remark on dB An asterisk indicates that the magnitude difference between components had to be computed from values expressed in different style in the original papers. --- dR Red Differential Magnitude A negative sign indicates that the "secondary" is fainter in the blue channel and brighter in the red. mag e_dR Error of dR mag n_dR Remark on dR (see note on n_dB) --- SAO SAO Number --- SAOsuf SAO Suffix --- NAME Other Name for Star --- MAG Magnitude mag Sp Spectral Type --- RUN Run Number of the Observation see note for data1.dat --- DAY Observation Date Day --- MONTH Observation Date Month --- YEAR Observation Date Year --- G Grade see notes for data1.dat --- n_G Remark on G see notes for data1.dat --- SEP Vector Separation marcsec e_SEP Computed Error of Vector Separation marcsec n_SEP Remark on SEP (see note on n_G) --- PA Position Angle see notes for data1.dat deg n_PA Remark on PA (see note on n_G) --- SL Limb Slope --- n_SL Remark on SL (see note on n_G) --- e_SL Error of SL --- dB Blue Differential Magnitude mag e_dB Error of dB mag n_dB Remark on dB see notes for data1.dat --- dR Red Differential Magnitude see notes for data1.dat mag e_dR Error of dR mag n_dR Remark on dR (see note on n_dB) --- DM DM Number --- NAME Other Name for Star --- MAG Magnitude mag Sp Spectral Type --- RUN Run Number of the Observation see notes for data1.dat --- DAY Observation Date Day --- MONTH Observation Date Month --- YEAR Observation Date Year --- G Grade see notes for data1.dat --- n_G Remark on G see notes for data1.dat --- SEP Vector Separation marcsec e_SEP Computed Error of Vector Separation marcsec n_SEP Remark on SEP (see note on n_G) --- PA Position Angle see notes for data1.dat deg n_PA Remark on PA (see note on n_G) --- SL Limb Slope --- n_SL Remark on SL (see note on n_G) --- e_SL Error of SL --- dB Blue Differential Magnitude mag e_dB Error of dB mag n_dB Remark on dB see notes for data1.dat --- dR Red Differential Magnitude see notes for data1.dat mag e_dR Error of dR mag n_dR Remark on dR (see note on n_dB) --- Julie Anne Watko SSDOO/ADC 1995 Nov 03 I_110.xml 1112 I/112 Lowell Proper Motion Survey - Southern Hemisphere H L Giclas R Burnham Jr. N G Thomas Lowell Observatory Bulletin No. 164, ??? ??? 1978 1978LowOB...8...89G I/79 : Lowell Proper Motion Survey in Northernern Hemisphere (Giclas+ 1971) Giclas H.L., Burnham JR. R., and Thomas N. G. 1971, Lowell Proper Motion Survey, Northern Hemisphere, The G Numbered Stars (Flagstaff: Lowell Observatory). Giclas H.L., Burnham Jr. R., and Thomas N. G. 1978, Lowell Proper Motion Survey, Southern Hemisphere Catalog 1978, Lick Obs. Bull. No. 164. Positional data Proper motions This catalog contains a summary of the Lowell Proper Motion Survey for the southern hemisphere as completed to mid-1978. The catalog gives the position, motion, magnitude, and color of 2758 stars from the Lowell program.

The material from which this catalog has been prepared is drawn from Lowell Observatory Bulletins, in which the data have been published from 1958 to 1978. The number of the specific Lowell Bulletin where the object was first identified and measured and a finding chart given is given in the eighth column of the catalog under the heading CHT. The first epoch plates were taken in connection with the trans-Neptunian planet search beginning late in the year 1929. The second epoch matching plates were taken as the blinking and measuring progressed, Therefore the difference in epoch increased from a minimum of 28 years at the beginning of the survey to 48 years as of the date of this catalog. At the inception of the program, a reasonable degree of completeness could be maintained for motions of 0.27"/year and larger. Later in the program the limit was lowered to include motions of 0.20"/year and larger. This catalog, therefore, is a combination of these two limits of motions; however, the percentage of plate regions with the smaller motion limit is much greater in this southern hemisphere catalog than in the northern hemisphere. The four plate regions around the south galactic pole are all measured to the lower limit of motion.

G Original G number assigned Byte 1 of the field always contains a G and byte 5 always contains a -. The number in bytes 2-4 is the plate number, while that in bytes 6-8 is the star number on the plate. Original G number assigned to the star on the plate region where it was first found. Stars that were subsequently found on later plates were assigned new G numbers; however, in this catalog all duplicate observations have been combined and averaged with the original G numbers retained. In cases where a close companion has been found on a later plate, the source of a finding chart prepared from that plate may be found in the identification chart field (ref2). When the catalog entry is a mean formed from two or more observations, the additional stars making up the mean are listed first in the References field (ref). --- flag Note in the printed catalog An asterisk (*) indicates that a note concerning the star appears in the Bulletin in which it was first published. The reference to the original report of the motion is as follows: ---------------------------------------------------- Volume Page No. Year G Region ---------------------------------------------------- IV 136 102 1959 G1 -G50 V 61 112 1961 G51 -G100 VI 1 120 1964 G101-G150 VI 103 122 1964 G151-G160 VI 135 124 1964 G161-G170 VII 217 158 1972 G266-G269 VII 273 160 1973 G270-G271 VIII 9 162 1975 G272-G273 VIII 59 163 1978 G274-G275 --- RAh Right ascension hours (Equinox 1950) h RAm Right ascension minutes min RAs Right ascension seconds s DE- Declination sign (Equinox 1950) --- DEd Declination degrees deg DEm Declination arcminutes arcmin pm Annual total proper motion The annual proper motion in seconds of arc. The proper-motion vector is defined by the equation: pm = (mu(alpha)**2*cos(delta)**2+mu(delta)**2)**0.5 arcsec/yr pmPA Proper motion position angle The position angle of the reported motion in the usual notation from the north point through east, 0deg. to 360deg.. The position angle of pm is defined by the following set of equations: mu(alpha)*cos(delta) = pm*sin(pmPA); mu(delta) = mu*cos(pmPA) deg Pmag Estimated Photographic (blue) magnitude mag col Color class The estimated color class is on a scale from -2 (the bluest) to +4 (the very reddest) stars found. Almost all stars of color classes -2 and -1 have been subsequently identified from photometry or spectra as white dwarfs. Because there is such a wide variety of different types of objects among these motions, it is impossible to define a narrow relationship between these color classes and the conventional B-V and U-B colors. The table below is given with the warning that the true color of any one individual star may deviate from the mean value by as much as half a magnitude for stars redder than color class 0. --------------------------------- Color Class B-V U-B --------------------------------- -1 +0.11 -0.74 0 +0.26 -0.57 +1 +0.80 +0.33 +2 +1.30 +1.09 +3 +1.61 +1.18 --- X-id Other identifications Catalog entries are, in many cases, the combined means of measurements on two or more plate regions; in these cases, the additional G number(s) appear as the first entry(ies) in the Reference field. If a G number in the references carries an asterisk, but the field following the identification field (byte 9) does not, then the note on that star appears only in the Lowell Observatory Bulletin where the latter number was published. Following the G numbers, references to other proper-motion lists and catalogs are given, as identified in the reference key in the appendix of this document. --- LOBchart Identification chart reference The Lowell Bulletin number in which an identification chart of size 18 minutes of arc on a side is given for the star. The summary catalog was compiled from collections of data appearing in earlier Lowell Observatory Bulletins. There are no finding charts in the source reference, but they can be found in the original references given in the table of the Note on n_ID. --- Acronym Designation of catalog or list The references to other proper-motion catalogs and lists are identified by character prefixes, followed by the numerical designations of the objects in a catalog or list, according to standard astronomical usage. The prefixes are identified with their corresponding references. (Note: Not all of the identifiers listed actually appear in the catalog. The key is repeated from the Lowell Proper Motion Survey, Northern Hemisphere (Giclas, Burnham, and Thomas 1971) and some identifiers may only appear in that catalog.) Reference Sources (= in column Sep) The bibliographical sources that provided information for the catalog consist of references for the star designations in other catalogs and lists, plus references for general information. The general references are combined with some supplementary identification references in the source publications and that order has not been changed in the following sections. The information given below appears in the source reference and is repeated here for users who do not have ready access to that publication. Supplementary References (: in column Sep) The supplementary references include sources of some identifiers used in the catalog, plus general reference sources consulted during preparation of the catalog. --- Sep original list (=) or supplement (:) --- Text Text of Reference --- Julie Anne Watko SSDOO/ADC 1995 Dec 08 A tape copy of the G-numbered stars was kindly supplied by H.L. Giclas to CDS in January 1985. I_112.xml 1113A I/113A General Catalogue of 33342 stars B Boss Carnegie Inst. of Wash. Publ. 468 ??? ??? 1937 1937gcse.bookQ....B Fundamental catalog Positional data Proper motions Stars, fundamental The GC is a catalog of standard positions and proper motions for (all) stars brighter than magnitude 7, extending from the north to south celestial poles. Several thousand additional stars promising to yield reasonably accurate proper motions were included in the catalog. The objectives of the work were to provide standard positions and motions of accuracy limited only by the character and abundance of the observational material upon which the data were based and thus to provide a rich supply of data to promote research in many astronomical fields. The machine version of the GC includes both The Henry Draper Catalogue and Durchmusterung identifications for all stars, although the published GC contains only one or the other. The 1985 version corrected many errors present in a previous machine version and included probable errors for the positions and centennial proper motions (not present in the previous version). In this version decimal points have been aligned for all but a very few of the secular variations and third terms. These quantities are given with the same precision as in the printed catalog, and the coded spectral types have been omitted. The following quantities are included in the machine but not the published version: galactic coordinates and DM numbers. The following data are in the published but not the machine version: centennial increments of proper motion in right ascension and declination, probable errors of the right ascension and declination at 1950.0, and remarks. The documentation supplied with the machine catalog gives a byte-by-byte format description, indigenous catalog characteristics, code explanation tables, and changes incorporated to produce this and previous Astronomical Data Center versions.

GC Boss General Catalog (GC) number --- Vmag Visual magnitude, '9999' indicates variability number=1 All magnitudes are given to two decimal places in the computer-readable version. Magnitudes underlined in the published version of the catalog are not indicated on the computer-readable version. 0.01mag SpType Spectral type --- RAh Hours RA, equinox 1950.0, epoch 1950.0 h RAm Minutes RA, equinox 1950.0, epoch 1950.0 min RAs Seconds RA, equinox 1950.0, epoch 1950.0 s EpRA Mean epoch of RA observations number=4 The first two digits of the year are omitted. Thus 98.8 should be read 1898.8 and 05.3 should be read 1905.3. a AvarRA Annual variation of precession in RA number=3 The number of decimals can be smaller for positions close to one of the poles (see document) s/a SvarRA Secular variation in precession in RA number=3 The number of decimals can be smaller for positions close to one of the poles (see document) 0.1ms/a2 Term3RA Third term in precession in RA number=3 The number of decimals can be smaller for positions close to one of the poles (see document) us/a3 pmRA Proper motion in RA s/a DE- Sign Dec, equinox 1950.0 --- DEd Degrees Dec, equinox 1950.0, epoch 1950.0 deg DEm Minutes Dec, equinox 1950.0, epoch 1950.0 arcmin DEs Seconds Dec, equinox 1950.0, epoch 1950.0 arcsec EpDE Mean epoch of DE observations number=4 The first two digits of the year are omitted. Thus 98.8 should be read 1898.8 and 05.3 should be read 1905.3. a AvarDE Annual variation of precession in DE number=3 The number of decimals can be smaller for positions close to one of the poles (see document) arcsec/a SvarDE Secular variation in precession in DE number=3 The number of decimals can be smaller for positions close to one of the poles (see document) 0.1mas/a2 Term3DE Third term in precession in DE number=3 The number of decimals can be smaller for positions close to one of the poles (see document) uarcsec/a3 pmDE Proper motion in Dec arcsec/a Remark Coded remarks number=2 Remarks are defined as follows: 0 = No remark given 1 = Spectrum given 2 = Aitken or Innes number given 3 = Aitken or Innes number given with each component having a separate GC number 4 = Other information given 5 = 1+2 6 = 1+3 7 = 1+4 8 = 2+4 9 = 3+4 - = 1+2+4 + = 1+3+4 --- DM Durchmusterung designation: catalog in bytes 101-102: 'BD', 'CD', 'CP' catalog number in bytes 103-110: SZZNNNNN component identification in bytes 111-112 BD supplement letter in byte 113 --- GLON Galactic longitude deg GLAT Galactic latitude deg HD Henry Draper Catalog (HD) number --- m_HD HD component/multiple code number=5 The HD component code takes the following values: 0 for single stars or brighter components of doubles with difference in visual magnitude > 0.3mag. 1 designates the brighter component, not necessarily A, for doubles with difference in visual magnitude <= 0.3mag 2 designates the fainter component, not necessarily B, for doubles with difference in visual magnitude <= 0.3mag 9 indicates that two successive HD numbers (HD and HD+1) refer to the same SAO star. --- e_RA Probable error in RA at epoch arcsec e_pmRA Probable error in RA proper motion 10mas/a e_DE Probable error in DE at epoch arcsec e_pmDE Probable error in DE proper motion 10mas/a GC Boss General Catalog (GC) number --- Field Field Changed --- Printed Old Value --- New Current Value --- adc.doc Documentation in plain ascii by ADC doc.tex ADC document in LaTeX Francois Ochsenbein CDS 1995 Oct 13 UNKNOWN UNKNOWN * See section 4 "Remarks and Modifications" in the document file (adc.doc or doc.tex), and the list of modifications in file "changes.dat" * A previous version is on the "Selected Astronomical Catalogs" Vol. 1 CD-ROM (October 1991), directory /astrom/gc * This standardized "ReadMe" document file was written in October 1995 at CDS (Francois Ochsenbein), using the ADC documentation written by Nancy G. Roman and Wayne H. Warren Jr. I_113A.xml 1114 I/114 Cordoba Durchmusterung J M Thome Resultados del Observatorio Nacional Argentino 16 Part I: -22deg to -32deg ??? ??? 1892 1892cdbp.book.....T J M Thome Resultados del Observatorio Nacional Argentino 17 Part II: -32deg to -42deg ??? ??? 1894 1894cdbp.book.....T J M Thome Resultados del Observatorio Nacional Argentino 18 Part III: -42deg to -52deg ??? ??? 1900 1900cdbp.book.....T J M Thome Resultados del Observatorio Nacional Argentino 21 Part I: -52deg to -42deg) ??? ??? 1914 1914cdbp.book.....T J M Thome Resultados del Observatorio Nacional Argentino 21 Part IV: -52deg to -42deg) ??? ??? 1914 1914cdbp.book.....T J M Thome Resultados del Observatorio Nacional Argentino 21 Part II: -62 deg to -90deg) ??? ??? 1932 1932cdbp.book.....T J M Thome Resultados del Observatorio Nacional Argentino 21 Part V: -62 deg to -90deg) ??? ??? 1932 1932cdbp.book.....T Surveys Durchmusterungen The "Cordoba Durchmusterung" (CD, Thome 1892-1932) is a visual survey of southern stars in the declination zones -22 to -89 deg, carried out as an extension to the "Bonner Durchmusterung" (BD) catalogs of Argelander (1859-1862) (see also Kuestner 1903) and Schoenfeld (1886). It contains 613959 records for stars brighter than 10.0 magnitude.

The goal of the survey was to obtain a position and estimated visual magnitude for every star down to 10.0 magnitude inclusive, but the faint limit was confirmed from comparisons with other catalogs, to be somewhat below 10. The positional uncertainties quoted in the original publications vary from +/- 0.42 sec and +/- 0.23 arcmin for zones -22 to -32 deg and +/- 0.33 sec, +/- 0.10 arcmin for zones -42 to -51 deg. The document originally prepared by Wayne H. Warren Jr., on which this document is closely based (adc.doc) contains substantial additional information.

cat The catalog prefix --- zonesign The sign of the declination zone --- zone The declination zone deg num The number of the star within the zone --- suppl star in corrigenda a, b, or c: star is added in the corrigenda; D: star is deleted in the corrigenda --- mag Estimated visual magnitude 20.0 = neb; 30.0 = var mag RAh Hours of right ascension, 1875 h RAm Minutes of right ascension, 1875 min RAs Seconds of right ascension, 1875 precision varies; tenths can be blank s DE- Sign of declination --- DEd Degree of declination, 1875 deg DEm Minutes of declination, 1875 arcmin zonesign The sign of the CP zone --- zone The CP zone --- num The CP number --- n_num Note on star number --- field The field changed --- old The printed value --- new The corrected value --- note Comments --- adc.doc The original ADC document Nancy G. Roman NSSDC/ADC 1994 Nov 12 Although the work was initiated and supervised by Jaylee M. Mead, Theresa A. Nagy and Wayne H. Warren Jr., punching could never have been begun and the project completed without the support and encouragement of the NSSDC Director James I. Vette. The keypunching was done at NSSDC by Beth Alexander, Carol Bergstrom and Margy Goodwin, while the monitoring software for the data transfer was written by Frank Barnes with contributions by Eugene Scarzafava, and data migration to tape was done by Charleen Perry with assistance and supervision by Ralph Post. Proofreading of individual zones was contributed by Scott Birney (Wellesley College), Richard Dietz (University of Northern Colorado), Mati Morel (Rankin Park, NSW, Australia), Theresa Nagy (ADC), Sidney Parsons (Space Telescope Science Institute), William Stein (U. S. Naval Surface Weapons Laboratory, Dahlgren, VA), George Wolf (Southwest Missouri State University), and the author. Additional zones were proofread at the ADC by summer students Paula Feldman and Kimberly Kniffen, who also assisted greatly with error checking, recording, and data correction. Checking and recording were also done at the ADC by Rajendra Nigam, Charleen Perry and the author. UNKNOWN UNKNOWN The data in the machine-readable "Cordoba Durchmusterung" were keypunched directly from the published catalog at the National Space Science Data Center (NSSDC). The original catalog had been microfiched earlier by photocopying and filming the entire printed version, and copies of the microfiche had been distributed to interested members of the astronomical community. Ten volunteers from the U.S. and Australia completed the proofing over the next three years. Individual zones from the complete preliminary tape were then transferred to disk storage and edited. This method was used to provide further checks where errors might be recognized during the correction process. as that zone was being processed. After the correction of all zones, the individual data sets were concatenated to a single magnetic tape file. This Users should particularly note that, due to corrections inserted from the corrigenda, the CD stars are not strictly in right ascension order within each zone; hence, if the catalog is sorted by R.A., e.g., for search purposes, some CD numbers will become disordered. On the other hand, if right ascension searching is to be performed, it will be necessary to sort the catalog by right ascension. All corrections made to the original catalog by incorporation of the corrigenda are presented in cdchg.dat where it is noted when stars have become disordered in right ascension following the changes. I_114.xml 1116 I/116 Cape Photographic Cat. 1950.0 J Jackson R H Stoy Ann. Cape Obs. 17 ??? ??? 1954 1954AnCap..17...40J J Jackson R H Stoy Ann. Cape Obs. 18 ??? ??? 1955 1955AnCap..18.....J J Jackson R H Stoy Ann. Cape Obs. 19 ??? ??? 1955 1955AnCap..19.....J J Jackson R H Stoy Ann. Cape Obs. 20 ??? ??? 1958 1958AnCap..20.....J R H Stoy Ann. Cape Obs. ??? ??? 1966 1966AnCap..21.....S Positional data Proper motions Magnitudes, photographic Photographic catalog This catalog includes most of the stars from the 1900.0 Cordoba Zone Catalogues B and C in the zone -30 deg. -35 deg. at the equinox of 1925.0. Some of the fainter Cordoba stars have been omitted in the rather crowded regions in the Milky Way. The aim was to provide accurate places for an average of 9 to 10 stars per square degree as a reference for a rereduction of the AG positions. Most of the stars have visual magnitudes between 7 and 10. Positions and proper motions have been supplied from the General Catalogue for those stars that were too bright for accurate measurement on photographic plates. The positions are on the FK3 system for the equinox of 1950.0. The probable errors of the positions are nominally +/- 0.15" in both right ascension and declination. That of the proper motions should not exceed +/- 1.4"/century, or +/-14 in the units in which the proper motions expressed in arc are given in the catalog.

Whenever possible, proper motions are derived by comparison with earlier visual observations but for many of the stars in the more southerly zones, no earlier observations exist. The magnitudes were determined from a series of in-focus photographs in both photographic and visual sensitivities. They are on the system defined by "Standard Magnitudes in the E Regions" (Cape Mimeogram No. 3, 1953). Although the resulting magnitudes are fairly close to this system, a small change of color equation with magnitude has not been completely eliminated. The transformation of the E-Region magnitudes to the UBV system is: B = SP(g) - 0.07 SCI + 0.20 V = SP(v) + 0.08 SCI - 0.06 B-V = 0.85 SCI + 0.26 Whenever possible, the spectral types are from the Henry Draper Catalogue or its extension. Types for a large number of other stars were supplied by the Harvard College Observatory. G. G. Cillie classified many stars between -30deg. and -40deg. on plates taken at Bloemfontein. Three errors were discovered after the catalog was typed. These have been corrected in this version. 3558 For Co. D. 30d 5059. read 30d 5061 7726 For Co. D. 32d10484, read 32d10488 10580 For spectral type F8, read K0

INDEX Index Number INDEX NUMBER ZONES (deg) ------------ ----------- 17A -30 to -35 18A -35 to -40 19A -52 to -56 20A -56 to -60 20B -60 to -64 21A -64 to -68 21B -68 to -72 21C -72 to -76 21D -76 to -80 22A -80 to -90 --- ID Catalog Identification Number --- rem Remark: a=supplemental star --- zone Durchmusterung Zone --- DM Durchmusterung Identification --- n_DM Remark on DM a = record has been inserted between successive DM numbers --- code Durchmusterung Code 20 = CD 40 = CpD --- RAh Right Ascension hours (1950.0) h RAm Right Ascension minutes min RAs Right Ascension seconds s DE- Declination sign (1950.0) --- DEd Declination degrees deg DEm Declination arcminutes arcmin DEs Declination arcseconds arcsec pmRA Centennial Proper Motion in RA cs/ha pmX Centennial Proper Motion RA*cos(DE) dam/ha pmDE Centennial Proper Motion in DE dam/ha Ep Epoch - 1900 a SPg Photographic Magnitude mag SPv Visual Magnitude mag CI Color Index mag Sp Spectral Type --- Julie Anne Watko SSDOO/ADC 1996 May 07 I_116.xml 1118 I/118 Elements of Minor Planets for 1986 Yu V Batrakov Izdatel'stvo Nauka, Leningrad ??? ??? 1985 1985 I/124 : Elements of Minor Planets for 1987 I/127 : Elements of Minor Planets for 1988 Batrakov Yu.V. 1985, Elements of Minor Planets for 1986. Leningrad: Izdatel'stvo Nauka. Ephemerides Minor planets Osculating elements of minor planets numbered by November 1, 1984, are given. Perturbations by major planets were computed at the ITA of the USSR Academy of Sciences on a BESM-6 computer using programs by N.K. Sumzina and V.A. Shor.

ID Minor planet number --- Eq Equinox=1950.0 a Ep Epoch = 1986 06 19 (JED 2446600.5) a anom Mean anomaly --- peri Argument of perihelion --- node Node --- incl Inclination --- e Eccentricity --- mdm Mean daily motion --- mag Absolute magnitude of the planet B(1,0) mag code The nine-figure perturbation code A "1" in the i-th position of the code means that the perturbations from the i-th major planet had been taken into consideration when determining the elements. --- opp Number of oppositions for improvement --- N Number of observations for improvement --- obs_yr1 First year First and last year of the time interval covered by the observations used for improvement a obs_yr2 Last year a rms Mean-root square error Root-Mean-Square variation between observed and predicted positions. --- ref1 Code for the source of the elements MP = Minor Planet Circular EP = Ephemerides of Minor Planets --- ref2 Page or Year for source of the elements MP => page EP => year --- name Name or preliminary designation of planet --- aut Author of the elements --- date six-figure code of the date: YYMMDD Six-figure code of the date when the set of elements have been computed and written on tape at the ITA -- Julie Anne Watko SSDOO/ADC 1996 Aug 15 UNKNOWN UNKNOWN by exchange from the Moscow Data Center I_118.xml 1119 I/119 Southern Durchmusterung E Schoenfeld Astronomische Beobachtungen auf der Sternwarte der Koeniglichen Rheinischen Friedrich-Wilhelms-Universitat zu Bonn 8, Part IV 1886 ??? ??? Bonn: Adolph Marcus 1886 Surveys Durchmusterungen The Southern Durchmusterung (SD) was computerized at the Centre de Donnees Astronomiques de Strasbourg and at the Astronomical Data Center at the National Space Science Data Center, NASA/Goddard Space Flight Center. Corrigenda listed in the original SD volume and published by Kuestner and Sticker have been incorporated into the machine file. In addition, one star indicated to be "missing" in a published list, and later verified, is flagged so that it can be omitted from computer plotted charts if desired. Stars deleted in the various errata lists have been similarly flagged, while those with revised data are flagged and listed in a separate table. This catalog covers the zones -02 to -23 degrees.

The Southern Durchmusterung (SD, Schoenfeld 1886, Becker 1949, Schmidt 1967) is a visual survey of stars in the declination zones -02 to -23 degrees, completed as an extension to Argelander's (1859-62) monumental Bonner Durchmusterung (BD). Schoenfeld's survey was carried out using the same methods as had been used for the BD, which Schoenfeld had helped to compile as one of Argelander's assistants. The goal of the survey was to extend the BD to declination -23 deg (a plan originally adopted by Argelander) with approximately the same magnitude limits, although the primary instrument was of larger aperture (159 mm) than the 78-mm telescope used for the BD. Thus, whereas the BD magnitude estimates extend to 9.4 mag with all fainter stars assigned a magnitude of 9.5, the SD magnitude estimates extend to 9.9 mag with all fainter stars assigned a magnitude of 10. As with the BD, the SD contains a rather large number of stars fainter than 10.0 mag and even occasionally as faint as 11 mag. Positions are given to the nearest 0.1 sec in right ascension and 0.1 arcmin in declination as in the BD. The document originally prepared by the ADC (adc.doc) contains substantial additional information.

cat The catalog prefix --- zonesign The sign of the declination zone --- zone The declination zone deg num The number of the star within the zone --- n_num Code Upper and lower case codes. All lower case letters represent supplemental (footnoted) stars added to the catalog via published corrigenda. Upper case letters and asterisks are flags that indicate changes to the original data or to the status of a star in the catalog. They have the following meanings: * Data have been corrected as a result of corrigenda, or there are special notes associated with the star. All changes are given in Section A, Table 4, with appropriate notes. D The star has been deleted in a later edition of the catalog. This was done by overstriking entries with horizontal lines. M The star was noted as "missing" in a list published by Pickering (1907). This entry (there is only one such star) was verified by R. A. Downes and at the ADC. --- mag Estimated visual magnitude 20.0 = neb; 30.0 = var; 40.0 = nova or nova?; 50.0 = cum (integrated magnitude estimate of a cluster of stars). mag RAh Right Ascension 1855 (hours) h RAm Right Ascension 1855 (minutes) min RAs Right Ascension, 1855 (seconds) s DE- Sign of declination --- DEd Declination 1855 (degrees) deg DEm Declination 1855 (minutes) arcmin zone The SD zone --- num The SD number --- n_num Code on star number --- field The field changed --- old The printed value --- new The corrected value --- note Comments --- adc.doc The original document Nancy G. Roman NSSDC/ADC 1994 Nov 12 Drs. Warren and Ochsenbein express appreciation to M. J. Wagner, M. Maslo, and R. Bonnet, who keyed the SD data to disk at the CDS using preprocessing software written and implemented by F. Ochsenbein. They thank Dr. R. A. Downes for bringing the cases of "missing" BD and SD stars to their attention and are grateful for the support of the CDS director, Dr. C. Jaschek, during the course of the work. This document is based on the original ADC document prepared by Wayne Warren, Jr. of the ADC and Francois Ochsenbein of the CDS. UNKNOWN UNKNOWN The data in the machine-readable Southern Durchmusterung were keyed directly to disk storage from the published catalogs at the Centre de Donnees Astronomiques de Strasbourg (-02 through -21 deg. zones) and at the Astronomical Data Center of the National Space Science Data Center at the NASA Goddard Space Flight Center (-01, -22 and -23 deg. zones). Most of the data entry work was done at the CDS, where the data were also verified. The ADC zones -01 and -23, although not often used for stellar designations (the BD is used in zone -01 and the Cordoba Durchmusterung in zone -23), were added for completeness. The three ADC zones were computerized and proofread by Wayne Warren Jr. All zones were carefully examined, checked for sequencing and record counts, reformatted, and merged in the correct order at the ADC, where the final catalog was assembled. The published corrigenda lists were cross checked against the reprinted editions (1949, 1967) of the catalog. The final catalog was run through a verification program that checked numerical sequencing of the SD numbers, monotonic increase in right ascension, and allowed data ranges. All cases where stars are out of RA order were checked in the original data to verify that their positions are as in the original catalog or the corrigenda. The final file is ordered north to south strictly by SD number, i.e., in the zone order -01, -02, ..., -23. Users should note, however, that all stars are not strictly in right ascension order within each zone. This is because individual stars are occasionally out of RA order in the original catalog and because of corrections inserted from the corrigenda. UNKNOWN UNKNOWN All changes made to SD data and known to Warren and Ochsenbein were incorporated into the present machine-readable version. Unlike the Bonner Durchmusterung, where there had been numerous stars added and deleted, changes in supplemental entries from version to version, and a large number of data corrections, the changes to the SD are relatively few. There were two stars added as supplementary entries ("a" suffix), two stars deleted, and one star published as "missing" by Pickering (1907) and subsequently verified by R. A. Downes of Applied Research Corporation. A small list of corrections was also included in the introduction to the original published catalog. These modifications to the printed catalog are flagged by codes in byte 11 of the affected records and are listed in sdchg.dat. I_119.xml 1121 I/121 Common proper motions stars in AGK3 J L Halbwachs Astron. Astrophys. Suppl. Ser. 66 131 1986 1986A&AS...66..131H Proper motions Stars, double and multiple The 326 common proper motion systems that have a ratio angular separation to proper motion smaller than 1000 years are in table1. The number of optical systems is expected to be around 4. Each system fills a 256 byte-length record that may also be considered as two 128 byte-length records for print-out edition. The 113 common proper motion systems that have a ratio angular separation to proper motion between 1000 and 3500 years are in table2. The number of physical systems is expected to be around 68. The presentation is the same as for table1. This table differs from the original printed version, since the the magnitude and the spectral type of the secondary component of the 47th system were corrected. The system 47 was also added to the notes.

Nseq sequential number of the system --- AGK2(A) number of the primary component --- HD/BD(A) HD or BD of the primary component --- ADS/IDS(A) ADS or IDS identification of the primary component --- Amag magnitude of the primary component mag n_Amag V when the magnitude is visual, P when it is photographic --- Sp(A) spectral type of the primary component --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin pm proper motion of the system mas/yr Id(A) other identification: Luyten Double Star (LDS) or cluster member --- Notes Note codes (see Notes sections below) --- AGK2(B) AGK2 number of the secondary component --- HD/BD(B) HD or BD of the secondary component --- ADS/IDS(B) ADS or IDS identification of the secondary component --- Bmag magnitude of the secondary component mag n_Bmag V when the magnitude is visual, P when it is photographic --- Sp(B) spectral type of the secondary component --- PA position angle of the secondary component deg Dist angular separation between the components arcsec rho/mu Ratio angular separation to proper motion, in 1000 years. kyr Id(B) Other identification of the secondary component --- CDS Catalogue Service CDS 1994 Oct 06 I_121.xml 1122 I/122 Bonner Durchmusterung F W A Argelander Bonner Sternverzeichniss, erste bis dritte Sektion, Astronomischen Beobachtungen auf der Sternwarte des Koeniglichen Rheinishen Friedrich-Wilhelms-Universitaet zu Bonn, Baende 3-5, ??? ??? 1859-62 I/119 : Southern part "Suedlicher Durchmusterung" (-02 to -23 degrees) I/114 : Cordoba Durchmusterung (-22 to -90 degrees) I/108 : Cape Photographic Durchmusterung (-18 to -90 degrees) Argelander, F. W. A. 1859-1862, Bonner Sternverzeichniss, erste bis dritte Sektion, Astronomischen Beobachtungen auf der Sternwarte des Koeniglichen Rhein., Friedrich-Wilhelms-Universitat zu Bonn, Bande 3-5. Becker, F. 1951, Bonner Durchmusterung, Noerdlicher Teil, Deklinations-Zonen -1 bis +89 grade Sternverzeichnis, dritte, berichtigte Auflage (Bonn: Ferd. Duemmlers Verlag). Chandler, S. C. 1896, Astron. J. 16, 145. Couteau, P., Fulconis, M., Ochsenbein, F., Wagner, M. J., and Maslo, W. 1983, Inf. Bull. CDS No. 25, p. 83. Giclas, H. L., Burnham, R. Jr., and Thomas, N. G. 1971, Lowell Proper Motion Survey, Northern Hemisphere, The G Numbered Stars (Flagstaff: Lowell Observatory). Kuestner, F. 1903, Bonner Durchmusterung des Noerdlichen Himmels, zweite berichtigte Auflage, Bonn Universitats Sternwarte (Bonn: A. Marcus und E. Weber's Verlag). Kuestner, F. 1908, Astron. Nach. 178, 33 (Nr. 4251). Kuestner, F. 1918, Astron. Nach. 206, 69 (Nr. 4929). Kuestner, F. 1925, Astron. Nach. 223, 309 (Nr. 5347). Luyten, W. J. 1979, 1980, New Luyten Catalogue of Stars with Proper Motions Larger than Two Tenths of an Arcsecond (Minneapolis: University of Minnesota). Luyten, W. J. and Hughes, H. S. 1980, Proper Motion Survey with the Forty- Eight Inch Schmidt Telescope. LV. First Supplement to the NLTT Catalogue (Minneapolis: University of Minnesota). Pickering, E. C. 1885, Harv. Ann. 14. Pickering, E. C. 1892, Harv. Ann. 23. Pickering, E. C. 1907, Astron. Nach. 175, 139. Pickering, E. C. 1913, Harv. Ann. 72. Schmidt, H. 1968, Bonner Durchmusterung, Noerdlicher Teil, Deklinations-Zonen -1 bis +89 grade Sternverzeichnis, vierte Auflage (Bonn: Ferd. Duemmlers Verlag). Sticker, B. 1935, Astron. Nach. 256, 341 (Nr. 6139). Sticker, B. 1936, Astron. Nach. 259, 187 (Nr. 6203). Sticker, B. 1938, Astron. Nach. 265, 127 (Nr. 6344). Upgren, A. R., Grossenbacher, R., Penhallow, W. S., MacConnell, D. J., and Frye, R. L. 1972, Astron. J. 77, 486. Wagner, M. J. 1984, Inf. Bull. CDS No. 26, p. 87. Wagner, M. J. 1986, Inf. Bull. CDS No. 30, p. 117. Warren, W. H. Jr. 1987, Inf. Bull. CDS No. 32, p. 67. Warren, W. H. Jr. and Kress, K. 1980, Astron. Data Center Bull. 1, 19. Surveys Durchmusterungen The Bonner Durchmusterung (BD, Argelander 1859-62, Kuestner 1903, Becker 1951, Schmidt 1968) is a visual survey of stars in the declination zones +89 to -01 degrees. The goal of the survey was to obtain a position and estimated visual magnitude for every star visible with the 78-mm Bonn telescope. Actual magnitude estimates were made and reported to 0.1 mag for all stars down to 9.5 mag, with fainter stars being assigned to 9.5. Positions are given to the nearest 0.1 sec in right ascension and 0.1 arcmin in declination.

The Bonner Durchmusterung (BD, Argelander 1859-62, Kuestner 1903, Becker 1951, Schmidt 1968) is a visual survey of stars in the declination zones +89 to -01 degrees performed by allowing the telescope to drift along the mean declination of each zone and recording the positions and magnitudes of stars crossing the transit line of each field. Actual magnitude estimates were made and reported to 0.1 mag for all stars down to 9.5 mag, with fainter stars being assigned to 9.5. The BD actually contains a rather large number of stars fainter than 10.0 mag. Positions are given to the nearest 0.1 sec in right ascension and 0.1 arcmin in declination. The catalog includes all corrigenda published in the original BD volumes have been incorporated into the machine file, along with changes published by Kuestner and Sticker following the 1903 edition. In addition, stars indicated to be "missing" in published lists and verified by various techniques are flagged so that they can be omitted from computer plotted charts if desired. Stars deleted in the various errata lists have been similarly flagged, while those with revised data are flagged and listed in a separate table. No other corrections or changes have been incorporated into the original data, e.g., from more modern positions and magnitudes or from comparison with other catalogs. The original document (adc.doc) contains substantial additional information.

cat The catalog prefix --- zonesign The sign of the declination zone --- zone The declination zone deg num The number of the star within the zone --- suppl Note a, b, or c: star is added in the 1903 or later editions * Data have been corrected as a result of corrigenda ? Existence of the star by Kuestner or Sticker D The star was deleted in a later edition by overstriking M The star was noted as missing by Chandler or Pickering --- mag Estimated visual magnitude 20.0 = neb; 30.0 = var; 40.0 = nova or nova?; 50.0 = integrated magnitude for a cluster mag RAh Right Ascension 1855 (hours) h RAm Right Ascension 1855 (minutes) min RAs Right Ascension, 1855 (seconds) s DE- Sign of declination --- DEd Declination 1855 (degrees) deg DEm Declination 1855 (minutes) arcmin zone The BD zone --- num The BD number --- suppl Supplemental designation --- field The field changed --- old The printed value --- new The corrected value --- note Comments 1 Star of approximately 13 mag at nominal position. 2 There is a "?" in the 1903 edition. No star could be found on the POSS prints or on the Vehrenberg Atlas Stellarum chart. 3 Star of approximately 12 mag at nominal position. 4 Candidate in field, but it is 3 arcmin north of the BD position. Star listed by Upgren et al. (1972) at right ascension an hour away from the BD position. 5 Faint star(s) in field, but "M" flag retained in record. 6 Possible variability noted by Kuestner (1918). 7 Existence also questioned by Kuestner (1908). 8 There is a "?" in the 1903 edition that was later removed by Kuestner (1918). 9 There is a "?" in the 1903 edition of the BD. 10 Non-BD star within 10 arcmin of nominal BD position. 11 Non-BD star within 10 arcmin of nominal BD position; existence questioned by Kuestner. 12 Non-BD star within 10 arcmin of nominal BD position. There is a "?" a "?" in the 1903 edition of the BD. 13 There is a question mark in the 1903 edition that was later removed by Kuestner (1918). There is a non-BD star within 10' of nominal BD position. --- adc.doc The original document Nancy G. Roman NSSDC/ADC 1994, modified CDS 20-Sep-1995 Nov 12 This immense project was successfully completed only through the combined efforts of the institutes and individuals listed above and the work of many persons within those institutes. The initial work at the Astronomical Data Center/NSSDC was begun and supervised by Drs. J. M. Mead, T. A. Nagy, and Wayne Warren, Jr. but the punching could never have been begun, nor the project completed without the support of the former NSSDC Director, Dr. James I. Vette. This support continued under Dr. James L. Green, and the Head of NSSDC's Central Data Services Facility, Dr. Joseph H. King. The NSSDC zones (+19 to -01 ) were punched by Beth Alexander, Carol Bergstrom, and Margy Goodwin, while monitoring software for data transfer was written by Frank Barnes and migration to magnetic tape was done by Charleen Perry under the supervision of Ralph Post. ADC software for the formatting of binary data and for the exact reproduction of published pages for proofreading was written by Wayne Warren Jr. but the actual proofing was accomplished by summer students Paula Feldman and Kimberly Kniffen, who also assisted greatly with error checking, recording, and data corrections. Zones +24 and +25 were keyed directly to disk, printed, and proofread by Warren, while B. N. Rappaport arranged for the keypunching of zones +23 to +20 by Syntronix, Incorporated, of Sherman Oaks, California, checked the data with his own computer programs and financed the work himself. The punching of zones +59 to +26 was accomplished at l'Observatoire de Nice by M. Fulconis, under the direction of P. Couteau, and their proofreading was done at the CDS by M. J. Wagner and W. Maslo. Zones +80 to +60 were keyed directly to disk at the CDS by M. J. Wagner, W. Maslo, and R. Bonnet, with preprocessing software written and implemented by F. Ochsenbein. Zones +25 and +24 were also computerized at the CDS and used to check the data prepared at the Astronomical Data Center. Finally, the compilers thank Dr. R. A. Downes of Applied Research Corporation for bringing the "missing" stars to our attention, for supplying a complete list of the stars, and for rechecking certain questionable cases. This document is based on the original ADC document prepared by Wayne Warren Jr. UNKNOWN UNKNOWN The data in the machine-readable Bonner Durchmusterung were keypunched directly from the published catalogs through the collaborative efforts of personnel at l'Observatoire de Nice, the Centre de Donnees Astronomiques de Strasbourg, the National Space Science Data Center at the NASA/Goddard Space Flight Center, and with the help of B. N. Rappaport, then at the NASA Jet Propulsion Laboratory. The following is the distribution of the work: Zones Location +89 to +60 Centre de Donnees Astronomiques de Strasbourg (CDS) +59 to +26 L'Observatoire de Nice +25 to +24 National Space Science Data Center (also CDS) +23 to +20 B. N. Rappaport (+23 also done at CDS) +19 to -01 National Space Science Data Center (+14 also done at Nice) Zones +89 to +60 were also verified at the CDS and zones +59 to +26 were proofread there, while the remaining zones were proofread at the Astronomical Data Center. Redundant zones were compared by computer and appropriate corrections were made. All zones were carefully examined, checked for sequencing and record counts, reformatted, and merged in the correct order at the ADC, where the final catalog was assembled. The supplemental entries were incorporated into the ADC/NSSDC and Rappaport zones from an earlier catalog prepared by Warren and Kress (1980) or used to check existing supplemental entries in the Nice and CDS zones. The published corrigenda lists were cross checked extensively against the reprinted editions of the catalog for preparation of the tables in the appendix of this document. Apparent discrepancies were checked on the BD charts and on the prints of the Vehrenberg Atlas Stellarum. The final catalog was run through a verification program that checked numerical sequencing of the BD numbers, monotonic increase in right ascension, and allowed data ranges. All cases where stars are out of RA order were checked in the original data to verify that their positions are as in the original catalog. The final file is ordered north to south strictly by BD number, i.e., in the zone order +89; +88; ...; -01. Users should note, however, that all stars are not strictly in right ascension order within each zone. This is because individual stars are occasionally out of RA order in the original catalog and because of corrections inserted from the corrigenda. Thus, if the machine catalog is sorted by increasing RA, e.g., for search purposes, some BD numbers will become disordered. *(20-Sep-1995, F. Ochsenbein, at CDS): Three further corrections made on stars: BD+65 820 (was named BD+65 821), BD+65 821 (was named BD+65 821!). BD-00 1000 (a digit was missing in the DEm field) I_122.xml 1123 I/123 Lunar Occultations of IRAS Point Sources, 1986-1990 M Simon L Cassar W P Chen Astrophys. J. Suppl. Ser. 62 673 1986 1986ApJS...62..673S Infrared sources Occultations The Lunar Occultations of IRAS Point Sources lists objects in the IRAS Point Source Catalog that were occulted by the Moon during 1986-1990.

The occultation predictions were based on the formulae for the lunar ephemeris developed by Van Flandern and Pulkinnen (1979). The topocentric predictions from this code are accurate to about +/-30s.

IRAS IRAS Point Source Cat. Object Name --- yr1 Starting Year yr1 and yr2 are the starting and ending years of the interval during which geometric events occur for the object. Some of the objects for which the ending year indicated is 1990 may actually have events in subsequent years because times later than 1990 were not considered in the present work. For objects having two intervals during 1986-1990 in which geometric events occur, the second interval is indicated in the line following the first entry. a yr2 Ending Year yr1 and yr2 are the starting and ending years of the interval during which geometric events occur for the object. Some of the objects for which the ending year indicated is 1990 may actually have events in subsequent years because times later than 1990 were not considered in the present work. For objects having two intervals during 1986-1990 in which geometric events occur, the second interval is indicated in the line following the first entry. a flux12 Mantissa for 12 um Flux Density flux fields list the mantissa of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. Jy exp12 Exponent for 12 um Flux Density exp fields list the exponent of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. --- flux25 Mantissa for 25 um Flux Density flux fields list the mantissa of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. Jy exp25 Exponent for 25 um Flux Density exp fields list the exponent of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. --- flux60 Mantissa for 60 um Flux Density flux fields list the mantissa of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. Jy exp60 Exponent for 60 um Flux Density exp fields list the exponent of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. --- flux100 Mantissa for 100 um Flux Density flux fields list the mantissa of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. Jy exp100 Exponent for 100 um Flux Density exp fields list the exponent of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. --- q_flux12 Quality of flux12 flux fields list the mantissa of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. q_flux fields refer to the flux-quality flags at 12, 25, 60 and 100 um, as indicated in the IRAS Point Source Catalog: H = high-quality detection M = medium-quality detection U = upper bound --- q_flux25 Quality of flux25 flux fields list the mantissa of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. q_flux fields refer to the flux-quality flags at 12, 25, 60 and 100 um, as indicated in the IRAS Point Source Catalog: H = high-quality detection M = medium-quality detection U = upper bound --- q_flux60 Quality of flux60 flux fields list the mantissa of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. q_flux fields refer to the flux-quality flags at 12, 25, 60 and 100 um, as indicated in the IRAS Point Source Catalog: H = high-quality detection M = medium-quality detection U = upper bound --- q_flux100 Quality of flux100 flux fields list the mantissa of the 12, 25, 60 and 100 um flux densities, in Janskys, as given in the IRAS Point Source Catalog. q_flux fields refer to the flux-quality flags at 12, 25, 60 and 100 um, as indicated in the IRAS Point Source Catalog: H = high-quality detection M = medium-quality detection U = upper bound --- cat Catalog Number For an object for which an identification with an object listed in some other astronomical catalog is provided in the IRAS Point Source Catalog, the catalog number, following the conventions of the IRAS Point Source Catalog, is given. --- name Object Name in Other Catalog For an object for which an identification with an object listed in some other astronomical catalog is provided in the IRAS Point Source Catalog, the first object name, following the conventions of the IRAS Point Source Catalog, is given. --- rem Remark An asterisk appears where there is more than one identification with an object listed in another astronomical catalog. Only the first is indicated in cat and name. The rest may be obtained from the original catalog. --- Julie Anne Watko SSDOO/ADC 1996 Feb 09 We thank Dr. Simon for forwarding this catalog to the ADC. I_123.xml 1125A I/125A Combined Lick-Voyager Reference Star Catalogue D W Dunham Unpublished ??? ??? 1986 1986 Positional data The catalogue contains accurate equatorial coordinates for stars in several bands of sky against which cameras of Voyager spacecraft were pointed for observations in the regions of Jupiter, Saturn, Uranus and Neptune during the flyby. This catalogue is compiled by combining the four reference star catalogues for Voyager mission: Uranus-Voyager Reference Star Catalogue <I/115> Klemola A.R., Owen Jr. W.M. <Lick Obs., Jet Propulsion Lab. (1985)> Neptune-Voyager Reference Star Catalogue <I/140> Klemola A.R., Owen Jr. W.M. <Lick Obs., Jet Propulsion Lab. (1986)> Jupiter-Voyager Reference Star Catalogue <I/152> Klemola A.R., Morabito L., Taraji H. <Lick Obs. (1978)> (Corrections by Owen Jr. W.M., 1990) Saturn-Voyager Reference Star Catalogue <I/153> Klemola A.R., Taraji H., Ocampo A. <Lick Obs. (1979)> (Corrections by Owen Jr. W.M., 1990) Note however that the corrections applied in 1990 to the last two catalogue Jupiter-Voyager and Saturn-Voyager are not incorporated here.

DMsign DM zone sign, or Lick indicator: + or - : Bonner Durchmusterung C : Cordoba Durchmusterung L : Lick (non-DM) --- DMzone DM zone (without sign), or if Lick: 1=Jupiter, 2=Saturn, 3=Uranus-pre, 4=Uranus-post, 5=Neptune --- DMnum sequence number in DM (or Lick) zone --- Vmag V magnitude (in unit of 0.01mag.) 0.01mag RAh Right Ascension B1950 (hours) at Epoch h RAm Right Ascension B1950 (minutes) min RAms Right Ascension B1950 (seconds) ms pmRA proper motion in RA (0.001s/century) 0.01ms/a DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) at Epoch deg DEm Declination B1950 (minutes) arcmin DEcs Declination B1950 (0.01 seconds) 10mas pmDE proper motion in DE (0.01arcseconds/cent) 0.1mas/a Bmag B magnitude (0.01mag.) 0.01mag SCnum Lick source number, see remarks below. --- SAO SAO number <I/131> --- SpType spectral type (if given) --- e_RA error of RA (0.01arcseconds) 10mas e_pmRA error of pmRA (0.01arcseconds/century) 0.1mas/a e_DE error of DE (0.01arcseconds) 10mas e_pmDE error of pmDE (0.01arcseconds/century) 0.1mas/a Epoch epoch of RA and DE, 0.01years since 1900. 0.01a plx parallax (0.0001arcseconds) 0.1mas AGK3 AGK3 designation (zone in bytes 81-83, number in bytes 85-88) --- Francois Ochsenbein CDS 1995 Nov 02 UNKNOWN UNKNOWN * Catalogue provided by ADC, NASA/GSFC * 16-Jul-1993: RA and DE transformed by Dr K. Nakajima (Visiting Astronomer at CDS) * 30-Aug-1993: Errors communicated by S. Nishimura, Tokyo Data Centre: The star names in BD +1 zone are erroneous: for read + 1 0 +14 1641 + 1 0 +19 1769 + 1 0 +19 1805 + 1 0 +26 1677 + 1 1528 +21 1528 + 1 1596 +21 1596 + 1 1643 +19 1643 + 1 1725 +14 1725 + 1 1792 +23 1792 + 1 1793 +18 1793 Note also that there are two stars named "L 1 1". * 02-Nov-1995: The corrections mentioned above by S. Nishimura have been incorporated into 'A' version, as well as the following modifications (Francois Ochsenbein, CDS): => The second "L 1 1" was changed to "L 4 1" => The zone sign of AGK3 numbers were transformed into '+' and '-' (instead of 'N' and 'S') => All southern DM numbers were erroneously indicated 'C' (from Cordoba Durchmusterung); 'C' was replaced by '-' (Bonner Durchmusterung) when appropriate. UNKNOWN UNKNOWN (David Dunham, 1986 Oct. 16): E-terms have been added to the Uranus catalogs, so that these are included for all stars. In column 47-51, SCnum, the number is the sequential number if actual DM No.'s (not "L" in column 1) are in columns 1-8. This is also the case for Neptune catalog stars, for which no plate or other catalog ID's are available. Otherwise, an abbreviation of the Lick plate No. is in column 47-48, and the No. of the star on the plate in column 49-51, both right-justified (as are all "I n" fields). "9999" in B-mag. field means no B-mag. is available. SAO-only and AGK3-only stars in the Uranus catalogs, which were not on any Lick plate, were skipped. Stars in the Uranus-Gemini catalog were matched with the Jupiter catalog; for matched stars, Uranus data superseded Jupiter data whenever possible (Jupiter data was used in the construction of the Uranus-Gemini catalog at J.P.L.). For 16 of the matched stars, one catalog gave an AGK3 No. and the other didn't. 173 stars in the Uranus-Sagittarius catalog had no magnitude informations; I arbitrarily set V-mag. for these stars = 11.4, unless the star was in the Co.D., in which case, I set V-mag. = 10.4. Although the position information in the Neptune catalog should be good, it has not been cross-referenced to other catalogs, and the photometry has not been calibrated. What I have is a preliminary version sent by Arnold Klemola to me early in September. Unlimited distribution of the Neptune catalog needs to wait until more work is done on it. In the meantime, any further distribution of Neptune catalog data needs Klemola's approval, although I am confident that this will be readily granted for those using the catalogs for occultations. David Dunham 1986 Oct. 16 I_125A.xml 1128 I/128 Photographic Obs. Visual Double Stars E van Albada-van Dien E Panjaitan Astron. Astrophys. Suppl. 68 117 1987 1987A&AS...68..117V Stars, double and multiple This catalog contains the results of photographic observations of 248 double stars, obtained at the Bosscha Observatory at Lembang, Indonesia 1981-1983.

RAh Right Ascension (1900,2000) hours Where bytes 1-54 are blank, bytes 55-127 belong to the previous record. h RAdm19 Right Ascension (1900) deciminutes dmin RAdm20 Right Ascension (2000) deciminutes dmin DE- Declination (1900,2000) sign --- DEd Declination (1900,2000) degrees deg DEm19 Declination (1900) arcminutes DEd applies to both epochs of DEm. DEm values greater than 60 arminutes result. These do not indicate errors in the data. arcmin DEm20 Declination (2000) arcminutes DEd applies to both epochs of DEm. DEm values greater than 60 arminutes result. These do not indicate errors in the data. arcmin rem Remark * = Pair has been removed from the program --- ADS ADS number or name mentioned in IDS --- paren1 Parentheses --- mag1 Magnitude of primary component from IDS blank = Null 99.9 = Variable mag comma Comma separator --- mag2 Magnitude of secondary component from IDS blank = Null 99.9 = Variable mag Sp Spectral type from IDS --- Ep Mean Epoch of observations - 1900 a dRAcosDE Mean value of delta(RA) * cos(DE) arcsec e_dRAcosDE Standard error of delta(RA) * cos(DE) Standard errors are given in units of the last decimal given. --- dDE Mean value of delta(DE) arcsec e_dDE Standard error of delta(DE) Standard errors are given in units of the last decimal given. --- D Distance derived arcsec e_D Standard error of D Standard errors are given in units of the last decimal given. --- PA Position Angle at Ep deg e_PA Standard error of PA Standard errors are given in units of the last decimal given. --- nplates Number of plates --- nimages Number of images blank = Null 99.9 = Variable --- paren2 Parentheses --- Wt Sum of weights --- paren3 Parentheses --- note Notes N = Northern Declination --- Julie Anne Watko SSDOO/ADC 1996 May 10 I_128.xml 1129 I/129 Parallaxes and Proper Motions near SGP C A Murray R W Argyle P M Corben Mon. Not. R. Astron. Soc. 223 629 1986 1986MNRAS.223..629M J/AJ/103/514 : (I colour and spectroscopic observations of the stars) Galactic pole, south Parallaxes, trigonometric Proper motions Regional catalog The catalog contains 6125 stars brighter than B=17.5, V=17.0 in the south galactic cap. The data have been obtained using the UK Schmidt telescope between 1975 and 1981. The plates were measured on the GALAXY machine at RGO. External errors of the parallaxes range between -/+0.012 and -/+0.017 arcsec according to magnitude. Internal proper motion errors range from -/+0.006 and -/+0.008 arcsec. In addition to the positions, proper motions, and parallaxes, the photometric data include B and V. Nomenclature Notes: The stars from this catalogue are named "RGO" followed by the number in "RGO" column of "catalog" file.

Seq Running Number --- RGO Serial number in RGO files --- Bmag (photographic) mag Vmag (photographic) mag B-V (photographic) mag q_RGO Astrometric quality code number=1 The quality code is blank for satisfactory data; it takes otherwise the following basic values 1 : Abnormal errors in Series B 2 : Abnormal errors in Series A 4 : Inconsistent results between the two Series The remaining codes are combinations of these (e.g. 3 = 1 + 2) --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (minutes) min RAs Right Ascension B1950 (seconds) s DE- Declination B1950 (sign) --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (minutes) arcmin DEs Declination B1950 (seconds) arcsec pmX Proper motion in X ("/y) arcsec/a pmY Proper motion in Y ("/y) arcsec/a plx Trigonometric parallax (") arcsec e_pos Internal standard error of a position coordinate arcsec e_pm Internal standard error of a proper motion component (pmX or pmY) arcsec/a e_plx Internal standard error of trigonometric parallax (plx) arcsec Epoch Mean epoch of observation a chi2 Chi-squared (5 degrees of freedom) from combination of Series A and B --- Xpos Standard coordinate X referred to RA= 0h 53m, Dec=-28.0deg (B1950) arcmin Ypos Standard coordinate Y referred to RA= 0h 53m, Dec=-28.0deg (B1950) arcmin Rem An asterisk (*) in this column signifies a further identification in Table 9 --- Francois Ochsenbein CDS 1995 Nov 02 We sincerely thank Drs C.A. Murray and R. Martin for having provided the magnetic tape version to CDS in November 1986. UNKNOWN UNKNOWN * November 1986: Tape provided by C.A. Murray (RGO) to CDS * 29-Jun-1993: First standardized description at CDS I_129.xml 1130 I/130 LDS Catalogue: Doubles with Common Proper Motion W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1969 1969PMMin..21....1L W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1970 1970PMMin..25....1L W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1972 1972PMMin..29....1L W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1975 1975PMMin..40....1L W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1977 1977PMMin..50....1L W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1980 1980PMMin..55....1L W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1983 1983PMMin..64....1L W J Luyten Publ. Astr. Obs. Univ. Minnesota III, part 3 35 1987 1987PMMin..71....1L Proper motions Stars, double and multiple This catalogue contains all double stars with common proper motion discovered by Luyten since 1940 up to 1987 (references below). When Luyten had noticed that an entry was duplicated (ref. 8 and 9), only the former LDS number was kept in the data file but with the data given for the latter. The unique exception is LDS 6166, which is a duplicate of LDS 5662, but with an additional component. The systems classified as optical by Luyten were also rejected from the main data files. All the rejected data were put together in a separate file. All coordinates are for the equinox 1950; when the original publication gave another equinox (this is the case for ref. 1), the 1950-coordinates were calculated. The catalogue contains all the systems, sorted by increasing LDS numbers. Duplicate entries and optical systems listed by Luyten were rejected. The catalogue contains 6121 systems, including 87 triple and 1 quadruple systems. The number of records is thus 6210, since each triple system occupies 2 records and the quadruple system 3.

LDS LDS number number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- Mult 't' indicates a system is triple and 'q' it is quadruple. Then, the LDS number is the same for all entries. number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- RAh Right Ascension 1950 (hours) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. h RAm Right Ascension 1950 (minutes) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. min RAs Right Ascension 1950 (seconds) number=1 When the seconds are provided, the RAm fractional part is blank s DE- Declination 1950 (sign) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- DEd Declination 1950 (degrees) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. deg DEm Declination 1950 (minutes) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. arcmin mR1 Photographic R magnitude of the primary component (99.9 = unknown) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. mag u_mR1 Uncertainty flag on mR1 number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- mB1 Photographic magnitude of the primary component (99.9 = unknown) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. mag u_mB1 Uncertainty flag on mB1 number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- color1 Color class of the primary component number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- mR2 photographic R magnitude of the secondary component (99.9 = unknown) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. mag u_mR2 Uncertainty flag on mR2 number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- mB2 photographic magnitude of the secondary component (99.9 = unknown) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. mag u_mB2 Uncertainty flag on mB2 number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- color2 Color class of the secondary component number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- pm Annual proper motion, number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. arcsec/a pmPA Direction (N to E) of the proper motion number=2 LDS 3543 has a value of 403deg (outside standard limits) deg Theta Position angle, see also Quadrant number=4 Theta, sep and Quadrant blank for LDS 149. LDS 1170 has a value of 440deg (outside standard limits) deg Sep Separation between components number=4 Theta, sep and Quadrant blank for LDS 149. LDS 1170 has a value of 440deg (outside standard limits) arcsec Quadrant Quadrant designation for ref.1 number=4 Theta, sep and Quadrant blank for LDS 149. LDS 1170 has a value of 440deg (outside standard limits) --- Remark Short remark and/or other identification number=3 the reasons for rejection are in bytes 81-91 in file "reject". A '*' refers to a remark (see 'Individual Remarks' below) The {Lambda} identifications given in ref.1 were not keypunched. --- Ref Reference code (see References section) number= Individual Remarks: LDS 372 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 555 Further observations made with the 36-inch reflector at Tucson render the existence of the faint companion extremely doubtful. LDS 846 A companion was announced by van Biesbroek at the Victoria Double Star Conference in 1956, 16th magnitude, red, 1130" distant in 67deg. As such it was included as gamma Leporis C in the LTT catalogue as LTT 2368. When the proper motion was published it was given as 0.63" in 210deg; our own measures on Palomar survey plates with an interval of 15 years, give 0.63" in 207deg thus fully confirming van Biesbroek's measure. However, the proper motion of gamma Leporis itself is given as 0.47" in 219deg, and its parallax as 0.122". The minimum separation of the C component from the brighter pair must therefore be of the order of 9000 astronomical units, and hence the parabolic velocity of the companion would at most be 0.7 km/sec, assuming a total mass of 2.5 for the triple system. The minimum observed velocity must be 6 km/sec, and hence there is no escape from the conclusion that, in spite of the close similarity in direction of the motions gamma Leporis and VBs 1 are not physically connected. LDS 1338 Close companion (14.9 mag, m, 34deg, 7") is optical. LDS 2095 Bright star is ADS 111, 6.0 - 6.2,88deg,172. LDS 2231 Bright star is VA 402. LDS 2721 These are the pr, and nf, of a triangle, brighter star in between. LDS 2730 If this is a physical pair, the separation is of the order of 20,000 a.u. LDS 2842 br star. =ADS 2481,optical? LDS 3035 angles increasing LDS 3097 BC maybe physical but A seems to have a larger motion LDS 5175 angles decreasing about 1deg/yr. --- J.-L. Halbwachs, F. Ochsenbein CDS 1997 Feb 04 UNKNOWN UNKNOWN Keypunched at CDS in 1987 * 15-Jun-1994: Corrected a few errors (existing in the publication) LDS 3593: third decimal place of proper motion (pm) set to blank LDS 4309: "+" embedded in DEm LDS 4871: RAm was -1 LDS 5644: secondary magnitudes were 18.,0 19.1 LDS 5679: third decimal place of proper motion (pm) set to blank LDS 5999: third decimal place of proper motion (pm) set to blank * 04-Feb-1997: ReadMe file standardized, and disentangled Quadrant from Theta values in data files * 19-Sep-1997: a few bad magnitude values (above 90.0) corrected in both main and rejected files. I_130.xml 1134 I/134 A New List of Trapezium-Type Multiple Systems G N Salukvadze Byull. Abastumani Astrofiz. Obs. No. 49, pp. 39-68 ??? ??? 1978 1978AbaOB..49...39S Stars, double and multiple This catalogue is based on the following works: 1 - G.N.Salukvadze, Abastumanskaya Astrofiz.Obs., Bull.49,39 (1978): A new list of trapezium-type multiple systems. and 2 - G.N.Salukvadze, Astrofizika 14 (1), 57 (1978): The catalogue of trapezium-type multiple systems. This catalogue of trapezium-type multiple systems was compiled on the basis of the index-catalogue of visual binary stars (IDS) (Jeffers et al., 1963). At the period of compilation of the Abastumani Catalogue, the IDS was the most complete catalogue concerning not only stars, but also the data on double stars. Besides giving relative positions, the IDS presents the coordinates at 1900 and 2000 epochs, as well as in most cases magnitudes, spectral classes and proper motions. The IDS contains all double and multiple stars from the North to the South poles with relative positions published up to the end of 1960, their total number being 64247. In order to select optimum value of K (ratio of the largest to the smallest distances among the components), which is the main criterion for relating a multiple star to the trapezium type, the dependence of the observed trapezia number on the K value has been analysed, and the value 2.6 adopted for it. To exclude optical components, upper limits for the distances of faint components to the main star have been introduced, and the components fainter than 12.5 mag. were excluded altogether (Salukvadze, 1978). The catalogue of trapezium-type multiple systems contains 412 trapezia, for which spectral classes in the MK system have been specified, after examining all main spectral catalogues (Jaschek et al., 1964; Kennedy et al., 1974; Hauck et al., 1975; Cruz-Gonzales et al., 1974; Lindsey et al., 1968). This was done for 100 systems, including 65 stars of O and B spectral classes. The following data on trapezia are given in the catalogue: positional angles and distances, magnitudes and spectral classes according to HD as well as MK, and the ADS and BD identification number of the main star. On the basis of the probability, deduced by Ambartsumian (1954), the number of pseudotrapezia was estimated, that is, the number of multiple stars, which in fact have no trapezium-type configurations, but are observed as trapezia as a result of their projection on the celestial sphere. The number of estimated pseudo-trapezia is 167. It should be mentioned that among 59 trapezia, the main components of which are of the O-B2 spectral class, there are only 5 pseudotrapezia. This enables us to maintain that there is a considerable percentage of real trapezia among the ones of mentioned spectral classes. Evaluation of the number of optical systems, formed as a result of the appearance of background stars in circles, which are determined by the upper limits of components' distances, led to their insignificant number - 9. The main star of the trapezium-type multiple system generally occupies 72 bytes and is marked by an asterisk (*) in the first and 72nd bytes. For each component of multiple systems 72 bytes were also taken, but, unlike the main star, the component's record is not marked by an asterisk (*), and the data for it is contained in bytes 17-39, which are: designation of components, relative positions and magnitudes of stars in trapezia.

main1 Denotes a main star --- N Ordinal number --- RAh1900 RA Hours (1900.0) h RAm1900 RA Minutes (1900.0) This field is listed to an accuracy of 0.1 minutes of time. 0.1min DE-1900 Dec Sign (1900.0) This field uses the uncommon values N-NORTH, S-SOUTH instead of + or -. --- DEd1900 Dec Degrees (1900.0) deg DEm1900 Dec Minutes (1900.0) The values are in arcminutes according to the IDS Catalogue. Sometimes these values are greater than 60. arcmin comp Designation of components --- PA Positional angle of a component relative to the main star deg sep Distance of a component to the main star arcsec Mvmain Magnitudes of the main star mag Mvcomp Magnitudes of trapezium components mag SpIDS Spectral class of the main star according to IDS --- SpMK Spectral class of the main star in the MK system --- ADS ADS number --- DM Durchmusterung number --- main2 Denotes a main star --- James E. Gass SSDOO/ADC 1997 Jul 30 The author thanks professor V.A.Ambartsumian for valuable advice during the compilation of the catalogue of trapezium-type multiple systems, As well as his collaborators from the Abastumani Astrophysical Observatory M. Butikashvili and N. Kiselyova for the transfer of the Trapezia Catalogue on magnetic tape. I_134.xml 1142 I/142 Lunar Occultations of IRAS Point Sources 1991-2000 M Simon L Cassar W P Chen Astrophys. J. Suppl. Ser. 69 651 1989 1989ApJS...69..651C I/123 : Lunar Occultations of IRAS Point Sources, 1986-1990 IRAS Point Source Catalog. 1985, Joint IRAS Science Working Group (Washington, DC: GPO). Cassar L., Chen W.P. and Simon M. 1989, Astrophys. J. Suppl. Ser. 69, 651. Simon M., Cassar L. and Chen W.P. 1986, Astrophys. J. Suppl. Ser. 62, 673. Occultations Infrared sources A listing of objects in the IRAS Point Source Catalog (1985) that were or will be occulted by the Moon during 1991-2000 is presented. Objects from the IRAS PSC that will have geocentric occultations during the years 1991- 2000 were identified using procedures described in Simon et al. (1986). This list is a sequel to the list of occultations for the years 1986-1990 (ADC catalog 1123).

IRAS IRAS Point Source Cat. Object name If IRAS is blank, then record is a continuation for the star in the previous record. --- yr1 Beginning year a yr2 Ending year a flux12 12 um Flux density Jy flux25 25 um Flux density Jy flux60 60 um Flux density Jy flux100 100 um Flux density Jy q_flux12 Quality flag on flux12 H = high-quality detection M = medium-quality detection U = upper bound --- q_flux25 Quality flag on flux25 H = high-quality detection M = medium-quality detection U = upper bound --- q_flux60 Quality flag on flux60 H = high-quality detection M = medium-quality detection U = upper bound --- q_flux100 Quality flag on flux100 H = high-quality detection M = medium-quality detection U = upper bound --- cat Catalog number For an object for which an identification with an object listed in some other astronomical catalog is provided in the IRAS PSC, the catalog number, following the conventions of the IRAS PSC, is given in the cat field, and the object name in that catalog is given. Where there is more than one identification with an object listed in another astronomical catalog, an asterisk (*) appears in rem. In this case, only the first identification is indicated in cat and ID. The rest may be obtained from the original IRAS PSC. --- ID Star identification in cat --- rem Remark on multiple identifications --- Julie Anne Watko SSDOO/ADC 1996 Aug 21 I_142.xml 1143 I/143 Fourth Fundamental Cat and Suppl W Fricke A Kopff Veroeff. Astron. Rechen-Inst., Heidelb., No. 10 ??? ??? 1963 1963VeARI..10....1F W Fricke A Kopff Veroeff. Astron. Rechen-Inst., Heidelb., No. 11 ??? ??? 1963 1963VeARI..11....1F I/149 : Fifth Fundamental Catalogue (FK5) Part I (Fricke+, 1988) I/175 : Fifth Fundamental Catalogue (FK5) Extension (Fricke+ 1991) Positional data Proper motions Fundamental catalog Stars, fundamental The FK4 was an attempt to establish a fundamental system of stellar positions and proper motions for the 1950 equinox using as much position data as were available. Most of the stars are brighter than 7.0 mag. To increase the star density in some regions of the sky, positions and proper motions for additional stars were established on the same system. This catalog contains seven data files, six for different equinoxes (1950, 1955, 1960, 1965, 1970, and 1975) and one for the supplemental stars. The 1950 and 1975 files contain the complete FK4 catalog (1535 stars); the others contain only 52 polar stars. In addition to a header record, the primary catalog contains for each star an identification number; the magnitude (maximum for a variable star); a variability flag, the minimum magnitude for a variable or the magnitude of the secondary for a double star; the HD spectral type and the type for the companion or a second type for a variable star; the position and the change and acceleration of the position; the proper motion and its change with time; the mean epoch of the observations for both right ascension and declination; the standard deviations of the position and proper motion; the numbers of the star in the Boss General Catalog, the N30 catalog, and in the Durchmusterungs; and the parallax. The supplement has a flag to indicate duplicity but no information about variability or the second component. It has no information about the temporal change of the position and proper motion and does not list the N30 and Durchmusterung numbers. It also omits the mean epoch for the observations.

FK4 FK4 star number. --- mpv Photovisual magnitude. mag var If "V", then star is variable. --- mpv2 Fainter mag or 2ndary mag in binary number=1 If a range of magnitudes is given in the book, this contains '-' in 10 and the fainter mag. in 11-12 (F2.1). Similarly, if both components of a double star are catalogued, byte 10 contains '+' and the magnitude of the secondary is in 15-17 (F3.2). Normally 14-17 are blank. mag SpType HD spectral type --- SpType2 Second HD spectral type number=2 If both components of a double star are catalogued, byte 23 contains '+' and 24-26 contain the HD spectral type for the secondary. If the entry is for a single star whose spectrum varies, byte 23 contains '-' and 24-26 contain the second spectral type. Normally 23-26 are blank. --- RAh RA B1950 (hours) h RAm RA B1950 (minutes) min RAs RA B1950 (seconds) s CvarRA Centennial variation (RA) s/ha SvarRA 1/2 the secular variation in RA s/ha2 pmRA Proper motion in RA s/ha d(pmRA) Centennial variation of pmRA s/ha2 EpRA-1900 Epoch (RA) number=3 The first two digits of the year are omitted. (E.g. 1908.22 = 0822) a e_RAs Std dev in RA at mean epoch s e_pmRA Std dev in pm in RA, time sec per trop cy. s/ha DE- Declination sign --- DEd Declination B1950 (degrees) deg DEm Declination B1950 (arc minutes) arcmin DEs Declination B1950 (arc seconds) arcsec CvarDE Centennial variation (Declination) arcsec/ha SvarDE 1/2 the secular variation in Dec arcsec/ha2 pmDE Proper motion in Dec arcsec/ha d(pmDE) Centennial variation of pmDE arcsec/ha2 EpDE-1900 Epoch (Dec) number=3 The first two digits of the year are omitted. (E.g. 1908.22 = 0822) a e_DEs Std dev in Dec at mean epoch arcsec e_pmDE Std dev in pm in Dec, arc sec per trop cy. arcsec/ha GC GC Catalog number (Cat. <I/113>) --- N30 N30 Catalog number (Cat. <I/80>) --- DM Durchmusterung number number=4 Durchmusterung number has form DMSZZNNNNN, where DM='BD', 'CD' or 'CP', and S='+' or '-'. E.g. 'BD+28 4' --- plx Parallax of star. Usually blank arcsec --- File identifier: 0293 for this file. --- FK4 FK4Sup star number --- GC Boss GC Catalog number (Cat. <I/113>) --- mpv Photovisual magnitude. mag SpType HD spectral type. number=1 Byte 22 is the prefix (blank except for #3505, which is 'c'); 23 is the class; 24 is the subclass; and 25 is the suffix (usually blank, but may be 'p' or 'e'). Two stars have type ' Oe5'. --- double Double star indicator ('2'=double) --- RAh Right Ascension B1950 (hours) h RAm Right Ascension B1950 (min) min RAs Right Ascension B1950 (seconds) s pmRA Proper motion in RA, time sec per trop cy s/ha DE- Declination sign --- DEd Declination B1950.0 (degrees) deg DEm Declination B1950.0 (minutes) arcmin DEs Declination B1950.0 (seconds) arcsec pmDE Proper motion in Dec, arcsec per trop cy. arcsec/ha plx Parallax, arc seconds. arcsec fk4_desc.txt Original FK4 catalog description Vincent Kargatis SSDOO/ADF 1997 Jul 24 UNKNOWN UNKNOWN The original machine-readable catalog consisted of seven files broken down by left and right pages for 1950 and 1975, left and right pages for the circumpolar stars, and a file for the supplement. The catalog was supplied to W. M. Owen, Jr. of the Jet Propulsion Laboratory (JPL) in January of 1989. Modifications to the data and format were made at JPL to correct miscellaneous errors, convert old BCD coding to ASCII representation, add Durchmusterung numbers and trigonometric parallaxes, and combine the left and right pages to single files containing one logical record per object in a uniform format. The revised catalog was then returned to the ADC at NASA GSFC, where the descriptive file (also prepared mostly at JPL) was modified. (The logical record length of the Supplement file was changed from 80 bytes to 55 bytes per record at the ADC because bytes 56-80 were blank.) The revised catalog was then archived permanently. * on ADC CD-ROM Volume 1 (October 1991), directory /astrom/fk4 * 24-Jul-1997: Added standardized ReadMe. I_143.xml 1144 I/144 First, Second and Third Herstmonceux Cats, 1950.0 R H Tucker M E Buontempo P Gibbs R H D Swifte R. Greenwich Obs. Bull. No. 189 ??? ??? 1983 1983N84-18125.....T Positional data Proper motions These catalogues contain the results of observations of stars made at the Royal Greenwich Observatory (Herstmonceux) with the Cooke Transit Circle from 1957 October 22 to 1980 November 18.

cat Catalogue label The following examples demonstrate the format of this field. 1HX502 = First Catalogue, part two 3HX504 = Third Catalogue, part four --- name Star name or number in cat --- Hxnum Herstmonceux number --- Hxc Herstmonceux culmination --- RAh Right Ascension (1950.0) hours h RAm Right Ascension (1950.0) minutes min RAs1 RA (1950.0) seconds: Herstmonceux Observed coordinates for epoch of observation, referred to the equinox of 1950.0, on 1. the Herstmonceux system of star places or 2. the FK4 system of star places The values in these fields are sometimes given greater than 60 (arc)seconds. To find the coordinates in such a case, add one to the (arc)minutes and subtract 60 from the (arc)seconds. The RAm (or DEm) value given applies to whichever RAs (or DEs) value is smaller. This occurs as a result of using one RAm (or DEm) value to describe two different systems and does not indicate errors in the data. s RAs2 RA (1950.0) seconds: FK4 system Observed coordinates for epoch of observation, referred to the equinox of 1950.0, on 1. the Herstmonceux system of star places or 2. the FK4 system of star places The values in these fields are sometimes given greater than 60 (arc)seconds. To find the coordinates in such a case, add one to the (arc)minutes and subtract 60 from the (arc)seconds. The RAm (or DEm) value given applies to whichever RAs (or DEs) value is smaller. This occurs as a result of using one RAm (or DEm) value to describe two different systems and does not indicate errors in the data. s EpRA Epoch of RA: Year-1900 (F6.3) a DE- Declination (1950.0) sign --- DEd Declination (1950.0) degrees deg DEm Declination (1950.0) arcminutes arcmin DEs1 DE (1950.0) arcseconds: Herstmonceux arcsec DEs2 DE (1950.0) arcseconds: FK4 system arcsec EpDE Epoch of Declination: Year-1900 a PlxRA Parallax factor RA AU PlxDE Parallax factor Dec AU o_RAh Number of Observations in R.A. --- o_DEd Number of Observations in Declination --- e_RAs1 Formal Standard Error RA Observed coordinates for epoch of observation, referred to the equinox of 1950.0, on 1. the Herstmonceux system of star places or 2. the FK4 system of star places The values in these fields are sometimes given greater than 60 (arc)seconds. To find the coordinates in such a case, add one to the (arc)minutes and subtract 60 from the (arc)seconds. The RAm (or DEm) value given applies to whichever RAs (or DEs) value is smaller. This occurs as a result of using one RAm (or DEm) value to describe two different systems and does not indicate errors in the data. arcsec e_DEs1 Formal Standard Error Declination arcsec rem Remark D = observation is a duplicate and appears elsewhere within catalogue. --- ADS ADS or IDS ADS number and component or IDS page number and component --- mag Magnitude mag n_mag V = Variable Magnitude --- Sp Spectral type(s) --- r_mag Source catalogue of mag and Sp S = SAO M = Mount Wilson GCRV Z = Robertson's ZC F = FK4 or FK4Sup A = AGK3R data from USNO Washington K = AGK3 V = Various sources --- GC Boss General Catalog number --- HD Henry Draper number --- DMzone Durchmusterung zone --- DM Durchmusterung number --- SAO Smithsonian Astrophys. Obs. Catalog number --- AGKzone AGK zone --- AGK AGK number --- n_AGK Remark on AGK suffix + indicates AGK2 number suffix * indicates Babelsberg number --- Julie Anne Watko SSDOO/ADC 1996 Aug 20 I_144.xml 1146 I/146 Positions and Proper Motions S Roeser U Bastian Astron. Astrophys. Suppl. Ser. 74 449 1988 1988A&AS...74..449R