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Table name: WD Records: 1279 Version: McCook & Sion, 1987 Spectral Band: Uband,Vband,Bband,OPT,Colour Index Kind of Object: White Dwarfs, Star Mode: Photometry,Astrometry,Proper Motion PreView: Coordinates: B1950
Name Type Meaning number c10 WD designation: 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 i4 Right ascension 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. dec i4 (see r_a) sp c6 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) r_sp c2 Reference to spectrum names c25 (see the list of abbreviations) mag i2 V magnitude, or photographic (see mag_d) mag_c uc1 A colon (:) for uncertain value mag_d c2 PG for photographic magnitude bmv i2 B-V bmv_c uc1 A colon (:) for uncertain value cclass c3 A color class from either the Lowell or Luyten proper motion surveys. umb i2 U-B umb_c uc1 A colon (:) for uncertain value r_ubv c2 Reference for UBV photometry v i2 Multichannel V magnitude v_c uc1 A colon (:) for uncertain value gmr i2 g-r from multichannel sperctrophotometric observations r_g c2 Reference for multichannel magnitudes ym i2 V determined from uvby photometry bmy i2 (b-y) index umby i2 (u-b) index r_uvby c2 Reference for uvby photometry amv i2 Absolute visual magnitude Mv amv_c uc1 A colon (:) for uncertain value pm i4 Total proper motion in arcsec per year pm_c uc1 A colon (:) for uncertain value pma i2 proper motion angle r_pm c2 Reference to proper motion rvel i4 Observed radial velocity uncorrected for solar motion and gravitational redshift r_rvel c2 Reference to Radial Velocity plx i2 Published values of the trigonometric parallax in arcsec e_plx i2 Mean error on plx in milli-arcsec r_plx c2 Reference of parallax note uc1 + is a note exists (see n_wd table) lines i1 Number of lines (records) for the White Dwarf Derived Values _ra F J2000 Right Ascension (epoch + equinox J2000) _de F J2000 Declination _lii F Galactic Longitude _bii F Galactic Latitude
The system uses :
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)
Type Characteristics
DA Only Balmer lines: no HeI or metals present.
DB HeI lines: no H or metals present.
DC Continuous spectrum, no lines deeper then 5spectrum.
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 information 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 com-positions.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 given.
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 Scie*nces,|p.276, (Prague).
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, LTTsee 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 : Iriarte, B., and Chavira, E. 1957, Bol.Obs.
Tonantzintla|y Tacubaya, 16, 3.
TS Chavira, E. 1958, Bol. Obs. Tonantzintla y Tacubaya, No.17.
PS Chavira, E. 1959, Bol. Obs. Tonantzintla y Tacubaya, 18, 3.
TON 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 Names: Refer to Fernandez, A., Lortet, M.-C., Spite, F. 1983,
Astron.& Astrophys. Suppl., 52, NO.4.
AMv
Computation of the Absolute Visual Magnitude :
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 = (11.43+-0.16) + (7.25+-0.75)(B - V ) - (3:42+-0.68)(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.
Aknowledgements
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.
References
"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 observations 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.
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.