Contents of: III/129/./intro.doc

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                               A CATALOGUE OF
                                WHITE DWARFS
                              GEORGE P. McCOOK
                               EDWARD M. SION
                                  JAN 1988

                              I.  INTRODUCTION

              The  first  edition  of  this  catalogue  was  published
          privately in  May 1977(McCook  and Sion  1977) as  Villanova
          University Observatory Contributions No.2 and contained less
          than  500  degenerate  stars.The  preface  to  that  edition
          provided  a  succinct   rationale  of  our   motivation  for
          preparing the catalog and is presented here verbatim:

             "The  number   of  newly  discovered  white   dwarfs  has
          increased  substantially since  the  the  appearance of  the
          first comprehensive  list by Eggen  and Greenstein  in 1965.
          The newly observed  objects when added to  the earlier lists
          comprise  a  sample  approaching   six  hundred  stars.  New
          spectroscopic, spectrophotometric  and photometric  observa-
          tions are being obtained by several active groups throughout
          the world. The volume of data is  enormous and much of it is
          dispersed throughout  the literature. Some  confusion exists
          with nomenclature  especially regarding multiple  names. The
          volume of  data and the nature  of its accessibility  in the
          literature  strongly  suggested  the   need  for  a  general
          comprehensive white dwarf catalogue.  While there is clearly
          no substitute for using the primary reference literature, it
          may prove useful in certain  applications for both observers
          and  theoreticians  to  have the  data  collected  into  one
          catalogue. We apologize in advance for the inevitable errors
          in  a catalogue  of this  size and  welcome corrections  and
          additions being  brought to our  attention for  inclusion in
          possible future editions".

              Since  the  appearance  of  the  First  Edition  of  the
          Villanova  Catalogue  of  Spectroscopically Identified White
          Dwarfs  ,the  number   of  newly  identified   spectroscopic
          degenerates has more than tripled due in a large part to the
          identification   of   several   hundred   new  spectroscopic
          degenerates at the 5.1m  Hale reflector by Jesse  Greenstein
          and through the Palomar-Green North Galactic Pole survey  of
          hot white dwarfs  by R. Green,  M. Schmidt, and  J. Liebert.
          In addition,  multi-channel spectrophotometry  by Greenstein
          and Green is now available  for over 500 white dwarfs  while
          over  300  stars  have  Stromgren  photometry  due mostly to
          J.Graham  ,G.   Wegner,  O.  Eggen,  M.  Bessel,  and   D.T.
          Wickramasinghe.  We decided in 1979 to postpone  publication
          of the second  edition until the  large sample of  hot white
          dwarfs  discovered  in  the  Palomar  Green  Survey   became
          available   for   inclusion.    In   doing   so  ,the second
          edition(McCook and Sion 1984)  presented a sample of  nearly
          1500  degenerate  stars  and  a  very  much  more   complete
          compilation of color and parallax data for the proper motion
          selected sample.

              It  was  felt  that  the  publication  of  the Villanova
          Catalogue  of  Spectroscopically  Identified  White  Dwarfs,
          Third Edition,  in  the  Astrophysical  Journal Supplement
          would greatly increase its user accessibility and offer  the
          opportunity to incorporate  revisions, corrections and  some
          additions to the second edition.

              The finalized Palomar-Green  sample of degenerate  stars
          (Green, Schmidt  and Liebert,  1986) contained  a number  of
          revised object and  spectral classifications resulting  from

          extensive follow-up spectroscopy of the many objects  having
          only single  discovery spectra  at lower  resolution.  As  a
          result  30  Palomar-Green  objects,  misclassified  as white
          dwarfs   have   been   deleted   from   our   catalogue,  16
          Palomar-Green objects reclassified as degenerate stars  have
          been added  and 276  Palomar-Green stars  were given revised
          spectral classifications.

              We have also  added a large  number of newly  identified
          degenerate stars  from the  following sources:  The Case Low
          Dispersion   Northern   Sky   Survey   (Sion,   Wagner   and
          Co-workers), the Kiso Ultraviolet Excess Survey (Wegner  and
          Co-workers),  the  Kitt  Peak  Downes  Survey  (Downes   and
          Co-workers), 5.1m  Palomar CCD  Spectroscopy by  Greenstein,
          and Faint Spectroscopy of Luyten Palomar Proper Motion Stars
          by Hintzen.   In addition,  a number  of new  parallaxes and
          photometric colors have been added, the descriptions of  the
          names entry  have been  expanded and  the notes  section has
          been significantly enlarged.


              As in the  First edition, we  have attempted to  include
          only    white    dwarfs    with    published   spectroscopic
          identification.  In  a very  few cases,  colors and  motions
          strongly indicate a white  dwarf, but no spectral  class has
          been as yet  assigned.  We have  included white dwarfs  that
          are components of essentially non-interacting binaries  (eg.
          Roche lobe  detached, short  and long  period systems) whose
          detected  photospheric  spectra  are  classifiable.   A  few
          examples illustrate the  morphological range of  such binary
          systems: HZ9, Sirius B, HZ43,  the DA component of the  mild
          Barium star Xi Ceti.  We have attempted to include all  data
          published  or  released  to  us  in  preprint  form prior to
          January 1987.

              Based  upon  input  we  have  received  from colleagues,
          content changes have been  introduced in the second  edition
          which  it  is  hoped  will  help  to maximize the scientific
          usefulness  of  the  second  edition.   A  new  white  dwarf
          spectral classification system proposed by Sion, Greenstein,
          Landstreet,  Liebert,  Shipman,  and  Wegner (1983) has been
          implemented and is briefly  described in the spectral  class
          entry section below.  An absolute visual magnitude has  been
          computed for each star with measured colors or trigonometric
          parallax and the computational procedure is described in the
          entry section  below.  In  addition, we  have eliminated the
          equivalent width entries from the second edition and we have
          retained the observed  radial velocity entry  but eliminated
          the  radial  velocity  corrected  for  solar motion and mean
          gravitational redshift.   A seven  digit WD  number has been
          adopted and the notes  section for white dwarfs  of greatest
          astrophysical  importance  has  been  expanded.  Names cross
          referenced with  WD numbers  have been  expanded to  include
          every white  dwarf name  used in  the catalogue.   The cross
          references are listed in appendix A.

                             III. THE ENTRIES IN TABLE 2

                   All entries  in table  2 except  coordinates, names  and
               absolute magnitudes  are followed  by a  reference number in
               brackets e.g.(41).  The reference  list can then be  used to
               identify the source of the catalogue entries.


              WD The first entry  contains a 'WD number',  a catalogue
          number containing the first  four digits of right  ascension
          followed by the sign and the first two digits of declination
          and a third digit in which minutes of declination have  been
          expressed as a fraction  of a degree.  Stars  with identical
          catalogue  numbers,  whether   binary  or  not,   have  been
          distinguished by using the designation .1 and .2 after their
          respective catalogue number.   The same distinction  is used
          for wide binary pairs.  The choice of the 'WD number' format
          was  made  with  the  idea  of  continuing  expansion of the
          catalogue as data accumulates.

    R.A. DEC       The second entry  contains the full right  ascension and
               declination  (1950.0)  adopted according  to  the  following
               order of  priority: Lowell  Observatory coordinates,  United
               States Naval  Observatory coordinates, Luyten  Proper Motion
               Survey coordinates.  For Bruce  Proper Motion  Survey stars,
               the coordinates may refer to epoch 1900.0 if no other proper
               motion name is listed.

    SP. CL.        The third entry lists the spectral type according to the
               new  system  described  by  E.M.  Sion, J.L Greenstein, J.D.
               Landstreet,J.  Liebert, H.L. Shipman, and G.A. Wegner (1983)
               , where a complete discussion may be found.  The system uses
               (1) an upper case D for degenerate; (2) an upper case letter
               for primary spectroscopic type in the optical spectrum;  (3)
               an upper case letter  for weaker or secondary  spectroscopic
               features, if  present, in  any part  of the  electromagnetic
               spectrum and (4) a temperature index from 0 to 9 defined  by
               10  X  i  (i  =  5040/T).   Additional symbols to follow the
               second  upper  case  letter  are  upper  case  P to indicate
               polarized magnetic  stars, H  for magnetic  stars showing no
               detectable polarization,  X for  peculiar or  unclassifiable
               spectra, and an  optional V to  denote the ZZ  Ceti stars or
               any other variable degenerate star.

                   Temperature-color   index   correlations   using   model
               atmospheres for DA and non-DA stars are available for multi-
               channel  spectrophotometric colors  (g-r); Stromgren  colors
               (u-b,  b-y);   and  broad  band   UBV  colors   (B-V,  U-B).
               Temperatures derived  from different model  atmosphere grids
               are generally very consistent.

                  We determine  the temperature  index by  using the color
               transformations based upon tables  1 and 2 and equations (9)
               and (10)  of Shipman  (1979).  The  transformation relations
               for non-DA stars are

                               (B-V) = 0.334 + 0.836 (g-r)
                               (b-y) = 0.286 + 0.553 (g-r).
                       For DA stars, the color transformations are:
                              (B-V) = 0.3336 + 0.5906 (g-r)
                              (b-y) = 0.2197 + 0.4485 (g-r).

                                     TABLE 1


                Spectral Type     Characteristics

                 DA               Only  Balmer  lines:  no  HeI  or  metals

                 DB               HeI lines: no H or metals present.

                 DC               Continuous spectrum, no lines deeper then
                                  5%  in any  part  of the  electromagnetic

                 DO               HeII strong: HeI or H present.

                 DZ               Metal lines only: no H or He lines.

                 DQ               Carbon   features,   either   atomic   or
                                  molecular  in  any  part of the  electro-
                                  magnetic spectrum.

                      *           An asterisk indicates additional informa-
                                  tion in the Notes section, appendix A.

                      b           The letter "b" Indicates a binary member.

              The definition of primary  spectral symbols is given  in
          table   1   according   to    the   Sion   et   al    (1983)
          classification.The  primary  symbols  may  be  combined  to
          designate atmospheres having hybrid compositions.For example
          a  DB4  star  showing  CaII  would  be  DBZ4,a DZ8 star with
          detectable H would be  DZA8,a DO1 star with  CIV(1550) would
          be DOZ1,et cetera.If more than one spectral class assignment
          has  been  made  and  cited  and  they are in agreement, the
          spectral type has  been converted to  the new system  and is
          followed by  the original  reference(s).  If  more than  one
          spectral class has been cited and they are in  disagreement,
          a spectral type converted to  the new system is given  based
          upon  our   assessment  of   the  spectral   resolution  and
          instrumental technology involved, but the old spectral types
          are retained  followed by  their references.   In many cases
          the primary classification reference has not been listed but
          may  be  easily  found  in  the secondary reference which is

    NAMES          The fourth entry contains  most of the names  that exist
               for each  star.  The  names are  listed below  with most  of
               their references  and an  extensive cross  reference, to the
               names used in Table 2, can be found in Appendix B.

    BPM        Bruce Proper Motion Survey
                    see reference list under Luyten
    C          Case
                    Stephenson, C.B. 1960,PASP, 72 ,387;1962,PASP, 74 ,610.
    CI20       Cincinnati
                    Porter, J.G., Yowell,E.J., and Smith,E.S. 1930,Publ.
                    Cincinnati obs.,No.20.
    CSO        Case Low Dispersion Survey
    CBS             Pesch, P., and Sanduleak, N. 1983,Ap.J.Suppl., 51 ,171
                    Sanduleak, N., and Pesch, P.1984,Ap.J. Suppl., 55 ,517.
                    Pesch, P., and Sanduleak, N.1985,Ap.J.Suppl., 60 ,543.
    EG         Eggen-Greenstein
                    See reference list under Eggen and Greenstein.
    F          Feige
                    Feige, J. 1958,Ap.J., 128 ,267.
    G,GD,GH    Lowell Names
                    see reference list under Giclas
    GL         Gliese
                    Gliese, W. Von. 1957,Katalog der Sterne Naher
                    als 20 parsek fur 1950.0, Heidelberg.
    GR         Greenstein
                    See reference list under Greenstein.
    GW         Greenwich
                    Astrographic Catalogue 1900.0 Greenwich Section,Vol.3
                    +64 to +90, F.W.Dyson,1914.
    HE         Hertzprung
                    Hertzsprung,E. 1918,A.N., 207 ,171.
    HL         Tonantzintla
                    Haro,G. and Luyten,W.J.1960,Bol. Obs.
                    Tonantzintla y Tacubaya,No.29,16.
    HZ         Humason-Zwicky
                    Humason, M., and Zwicky, F. 1947,Ap.J., 105 ,85.
    K1         Kohoutek (K1-16)
                    Perek, L., and Kohoutek, L.
                    Catalogue of Galactic Planetary Nebulae 1967,Academia
                    publ. house of the Czechoslovak Academy of Sciences,
               Karpov (K1-12)
                    Karpov, B.G. 1937,Pub.A.S.P., 49 ,146.
    KUV        Kiso
                    Kondo, M., Watanabe, E., Yutani, M., and
                    Noguchi, T. 1982,Publ.Astron.Soc.Japan, 34 ,541.
                    Noguchi, T., Maehara, H., and Kondo, M. 1980,Ann.Tokyo
                    Astr.Obs.,Ser.2, 18 ,55.
                    Kondo, M., Noguchi, T., and Maehara, H., 1984,Ann.Tokyo
                    Astr.Obs.,Ser.2, 20 ,130.
    KPD        Kitt Peak Downes
                    Downes, R. 1986,Ap.J.Suppl. 61 ,569.
    L,LB,LP    Luyten Names
    LDS,LHS,LTT     see reference list under Luyten

    MK         Markarian
                    Markarian,B.E.,and Lipovetski,V.A. 1971,
                    Astrofizika, 7 ,511.
    PB         Palomar-Berger
                    Berger, J., and Fringant, A. M. 1977,Astr.Ap.Suppl.,
                     28 ,123 and subsequent papers.
    PG         Palomar-Green
                    Green, R.F., Schmidt, M., and Liebert, J.W.
                    1986,Ap.J.Supp., 61 ,305.
    PHL        Tonantzintla
                    Haro,G. and Luyten,W.J.1962,Bol. Obs.
                    Tonantzintla y Tacubaya,3,No.22.
    R          Ross
                    Ross,F.E. 1925-1939,A.J., 36-48 .
    RB RWT     Rubin
                    Rubin, V.C., Westphal, D., and Tuve, M.
                    1974,A.J., 79 ,1406.
    SA         Basle Halo Program
                    Steppe,H.1978,Astr.Ap.Suppl., 31 ,209.
    SB         Slettebak and Brundage
                    Slettebak,A. and Brundage,R.K.1971,A.J., 76 ,338.
    TC         Tonantzintla
    TON             Iriarte, B., and Chavira, E. 1957,Bol.Obs.
    TPS             Tonantzintla y Tacubaya,16,3.
    TS              Chavira, E. 1958,Bol. Obs. Tonantzintla y
                    Chavira, E. 1959,Bol. Obs. Tonantzintla y
                    Philip,A.G.D. and Sanduleak,N.1968,Bol. Obs.
                    Tonantzintla y Tacubaya,4,No.30.
    US         Usher
                    Usher, P. D. 1981,Ap.J.Suppl., 46 ,117 and
                    subsequent papers.
    VB         Van Biesbroeck
                   Van Biesbroeck, G. 1961,A.J., 66 ,528.
    V Ma       Van Maanen
                    Van Maanen, A. 1938,Ap.J., 88 ,27.
    VR         Van Rhijn-Raimond
                    Van Rhijn, P.J. and Raimond, J.J. 1934,M.N.R.A.S., 94 ,508.
    W          Wolf
                    Wolf, M. 1919,Sternwarte zu Heidelberg,1,no.10,
                    A.N., 209-236 ,1919-1929.
    Other      Other Names--Refer to Fernandez,A.,Lortet,M.-C.,Spite,F.
                    1983,Astron.Astrophys.Suppl., 52 ,NO.4.

    WIDE BAND      Entry five contains published values of wide band UBV
    V B-V U-B      photometry. The V  magnitude is listed followed  by B-V,
               U-B  and the  reference number.  If  the star  has not  been
               observed on  the UBV  system, a  photographic magnitude  and
               color class (CC)  is given from either the  Lowell or Luyten
               Proper Motion Surveys. Photographic magnitudes are indicated
               by a PG following the magnitude in the V column.

    MC  MC         Entry  six  contains  multi-channel   spectrophotometric
    V   g-r        observations.  The  multi-channel  V magnitude is listed
                followed  by  the  multi-channel  color  and the  reference.

    STROMGREN      The seventh entry  lists  the  Stromgren,  narrow  band,
    y b-y u-b      photometry, y, b-y, u-b, and the reference.

    Mv        The  eighth  entry  lists  the absolute visual magnitude
          computed  from  either  trigonometric  parallax  or measured
          colors   according   to   the   following   priority:    (1)
          trigonometric    parallax    >    0".1    (2)  multi-channel
          spectrophotometric colors (3)  Stromgren narrow band  colors
          and (4) UBV photometry.  Exceptions to this priority  system
          are denoted with  numerical codes (0),(5),  and (6) and  are
          described  below.   If  measured  colors  do  not  exist, an
          absolute magnitude  was not  given.  For  all spectral types
          with (g-r) color index the following calibration formula due
          to Greenstein (1984) was employed:

                   Mv  =  13.033  +  3.114  (g-r)  -0.799  (g-r) 2

                   For  all  spectral  types  with  (b-y)  color index, the
               following calibration due to Green (1977) was adopted:
                                 Mv = 7.56 (b-y) + 11.50.

                   The  broad  band  calibrations are  those  of  Sion  and
               Liebert (1977).  For DA white dwarfs with B-V < 0.4:
                             Mv = 11.246 (B-V+1) 0.60  -0.045.
                             For non-DA stars with B-V < 0.4:
                             Mv = 11.916 (B-V+1) 0.44  -0.011.

                   If B-V   >  0.4  we used  the following  color-magnitude
               calibration due to Dahn et. al. (1982):
               Mv = (11.43q0.16)+(7.25q0.75)(B-V)-(3.42q0.68)(B-V) 2

              In a few cases where 3 or more measured parallaxes  from
          different sources are in agreement, exceptions were made  to
          the priority system  above.  Likewise, for  degenerate stars
          whose  spectra   exhibit  abnormally   strong  or   peculiar
          blanketing (e.g.   G47-18, GD  229, LP701-29)  and for  very
          cool white dwarfs (e.g.  LP131-66) the above priority system
          was  not  followed.Since  for  cool  white  dwarfs ,the blue
          colors(e.g.B-V,b-y,g-r)  yield  less  accurate   photometric
          parallaxes than the red colors(e.g.V-I,R-I),we have  adopted
          absolute magnitudes from the recent tabulation of cool white
          dwarfs  by  Liebert,Dahn  and  Monet(1987)  if  our   values
          differed by  more than  0.3 magnitudes  from theirs.   These
          values  are  denoted  by  numerical  code (6).  An extensive
          tabulation of red colors of  white dwarfs can be found  in a
          review by Eggen(1985 and references therein) while V-I color
          indices  are  available  from  the  USNO faint star parallax
          lists cited in this catalogue.  Likewise for the very hot DA
          stars where the blue-sensitive color-magnitude  calibrations
          are insensitive to temperature,we have used the values of  M
          derived from actual effective temperature determinations  as
          given for  example,by Fleming  et al.(1986)  and Holberg  et
          al.(1986).Here again however their values were adopted  only
          if  a  discrepancy  greater  than  0.3  mag. existed.  These
          values are denoted by  numerical code (0).  For  the hottest
          helium-rich  degenerates  the  photometric  parallaxes   are
          grossly inaccurate.For the DO and DOZ white dwarfs ,we  have
          replaced the M value  with the directly derivable  effective
          temperature in  units of  10 K.  Most of  the adopted values
          were  from  Wesemael  et  al.(1985)  and  are  indicated  by
          numerical code (5).

              A  discussion  of  the  dispersions  and analysis of the
          above calibrations is given in Sion (1979) and Sion  (1984).
          The  value  of  absolute  visual  magnitude is followed by a
          number 1,2,3 or 4  to indicate the method  of determination;
          (1) parallax; (2)  multi-channel color; (3)  Stromgren color
          and; (4) UBV color, or the  value is followed by (0), (5)  or
          (6) as described earlier.  Stars with hybrid classifications
          were generally not assigned a photometric parallax.

    MU THETA       The ninth entry contains the  published values of proper
               motion and  position angle followed  by the  reference.  The
               units are  seconds of arc per  annum for proper  motion, and
               degrees for the position angle.

    VR0            The  tenth  entry  lists the  observed  radial  velocity
               uncorrected for solar motion  and gravitational redshift and
               followed by the reference.

    PI ME          The final catalogue entry lists  the published values of
               the trigonometric parallax  in second of arc.  In most cases
               the parallax is followed by the reported mean error in units
               of 0.001 seconds of arc.

              We are grateful to  the many colleagues,too numerous  to
          mention,  who  communicated  data   to  us  in  advance   of
          publication, and who sent to us, corrections and suggestions
          concerning the format and content of this edition.  It is  a
          pleasure  to  express  our  deepest  gratitude to Drs. Jesse
          Greenstein and James Liebert for their valuable and detailed
          comments on  this edition  and to  Dr. Hugh  M. Van  Horn at
          whose  urging  we  decided  to  seek  publication in a major
          journal  instead  of  continuing  to  issue  the   catalogue
          privately.    We   thank   William   Harris,Kevin Hart,Brian
          McNamara, Robert Donahue,  Scott Wacker, Raj  Goyal, Matthew
          Lallo, and Joseph McMullin for their careful assistance with
          proofreading   and   data   compilation.    We    gratefully
          acknowledge the support  of the National  Science Foundation
          through  Grants   AST78-13396-A01-A02  and   AST85-17125  to
          Villanova University.


          Dahn,C.C., 1982,A.J. 87,426.
          Eggen,O.J. 1985,Pub.Astron.Soc.Pac. 97,1029.
          Fleming,T.,Green,R.F.,and Liebert,J. 1986,Ap.J. 308,176.
          Green,R.F. 1977,Ph.D. Thesis,Calif.Inst.Tech.
          Green,R F.,Schmidt,M.,and Liebert,J. 1986,Ap.J.Suppl. 61,305.
          Greenstein,J.L. 1984,Ap.J. 276,602.
          Holberg,J.B.,Wesemael,F.,and Basile,J. 1986,Ap.J. 306,629.
          Liebert,J.,Dahn,C.C.,and Monet,D.G. 1987,in preparation.
          McCook,G.P.,and Sion,E.M. 1977, A Catalogue of Spectroscopically
             Identified White Dwarfs,1st Edition,Villanova Univ. Obs.
             Contr. No.2.
          McCook,G.P. and Sion,E.M. 1977, A Catalogue of Spectroscopically
             Identified White Dwarfs,2nd Edition,Villanova Univ. Obs.
             Contr. No.3.
          Shipman,H.L. 1979,Ap.J. 228,240.
          Sion,E.M.,and Liebert,J. 1977,Ap.J. 213,468.
          Sion,E.M. 1979, IAU Colloq.  No. 53, White Dwarfs and Variable
             Degenerate Stars, ed.  H.M. Van Horn and V. Weidemann: Univ.
             of Rochester Press, p. 245.
             and Wegner,G.A. 1983,Ap.J. 269,253.
          Sion,E.M. 1984,Ap.J. 282,612..
          Wesemael,F.,Green,R.F.,and Liebert,J. 1985,Ap.J.Suppl. 58,379.