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J/AJ/135/1225       Parameters of the local white dwarfs        (Holberg+, 2008)

A new look at the local white dwarf population. Holberg J.B., Sion E.M., Oswalt T., McCook G.P., Foran S., Subasavage J.P. <Astron. J., 135, 1225-1238 (2008)> =2008AJ....135.1225H
ADC_Keywords: Parallaxes, trigonometric ; Stars, white dwarf ; Spectral types Keywords: stars: distances - stars: statistics - techniques: photometric - white dwarfs Abstract: We have conducted a detailed new survey of the local population of white dwarfs lying within 20pc of the Sun. A new revised catalog of local white dwarfs containing 122 entries (126 individual degenerate stars) is presented. This list contains 27 white dwarfs not included in a previous list from 2002, as well as new and recently published trigonometric parallaxes. In several cases new members of the local white dwarf population have come to light through accurate photometric distance estimates. In addition, a suspected new double degenerate system (WD 0423+120) has been identified. The 20pc sample is currently estimated to be 80% complete. Using a variety of recent spectroscopic, photometric, and trigonometric distance determinations, we re-compute a space density of 4.8±0.5x10-3pc-3 corresponding to a mass density of 3.2±0.3x10-3Mpc-3 from the complete portion of the sample within 13pc. We find an overall mean mass for the local white dwarfs of 0.665M, a value larger than most other non-volume-limited estimates. Although the sample is small, we find no evidence of a correlation between mass and temperature in which white dwarfs below 13000K are systematically more massive than those above this temperature. Within 20pc 25% of the white dwarfs are in binary systems (including double degenerate systems). Approximately 6% are double degenerates and 6.5% are Sirius-like systems. The fraction of magnetic white dwarfs in the local population is found to be 13%. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 76 122 The local sample of white dwarfs table2.dat 58 122 Local sample: physical parameters table3.dat 48 122 Local sample: distances table4.dat 74 37 Possible white dwarfs within 20pc refs.dat 146 36 References
See also: http://www.astronomy.villanova.edu/WDCatalog/index.html : WD Villanova catalog J/ApJS/133/413 : BVRIJHK photometry of cool white dwarfs (Bergeron+, 2001) J/A+A/378/556 : UVES/VLT spectra of white dwarfs (Koester+, 2001) J/ApJ/571/512 : Distances of white dwarf stars (Holberg+, 2002) J/ApJ/631/1100 : Atmospheric parameters of DA white dwarfs (Gianninas+, 2005) J/ApJS/161/394 : Low-luminosity companions to white dwarfs (Farihi+, 2005) J/ApJ/643/402 : Cool white dwarfs in the solar neighborhood (Kawka+, 2006) J/ApJS/167/40 : SDSS4 confirmed white dwarfs catalog (Eisenstein+, 2006) J/ApJ/654/499 : H-rich white dwarfs spectropolarimetric survey (Kawka+, 2007) J/AJ/134/252 : New nearby white dwarf systems (Subasavage+, 2007) J/ApJ/663/1291 : DZ stars in SDSS DR4 (Dufour+, 2007) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 2 A2 --- --- [WD] 4- 13 A10 --- WD WD number (HHMM+DDM.N, B1950) 14- 18 A5 --- n_WD [a-c, ] Note on WD (1) 20- 34 A15 --- OName Other name 36- 42 A7 --- SpType Spectral type 44- 49 F6.3 mag Vmag Visual magnitude 51- 56 F6.2 mas pi ?=- Trigonometric parallax 58- 62 F5.2 mas e_pi ?=- Parallaxe uncertainty 64- 68 A5 --- r_pi Reference(s) number for pi; see refs.dat file 70- 72 A3 --- Bin Binarity (2)
Note (1): Flags as follows: a = Not presently in the Villanova Catalog (http://www.astronomy.villanova.edu/WDCatalog/, Cat. B/wd) b = Preliminary trigonometric parallax indicates star well within 20pc c = New entery (not in Holberg et al., 2002, Cat. J/ApJ/571/512, HOS) Note (2): System as follows: b = Binary or multiple system, dd = double-degenerate system
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 2 A2 --- --- [WD] 4- 13 A10 --- WD WD designation (HHMM+DDM.N, B1950) 15- 16 A2 --- Comp Composition (He or H) 22- 26 I5 K Teff ?=- Effective temperature 28- 31 I4 K e_Teff ?=- Teff uncertainty 33- 37 F5.3 [cm/s2] logg ?=- Surface gravity 39- 43 F5.3 [cm/s2] e_logg ?=- logg uncertainty 45- 49 F5.3 Msun Mass ?=- Mass 51- 55 F5.3 Msun e_Mass ?=- Mass uncertainty 57- 58 I2 --- Ref ?=- Reference; see refs.dat file
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 2 A2 --- --- [WD] 4- 13 A10 --- WD WD designation (HHMM+DDM.N, B1950) 15- 19 F5.2 pc r.tr ?=- Trigonometric distance 21- 24 F4.2 pc e_r.tr ?=- r.tr uncertainty 26- 30 F5.2 pc r.ph ?=- Photometric distance 32- 35 F4.2 pc e_r.ph ?=- r.ph uncertainty 37- 41 F5.2 pc r ? Final adopted distance 43- 46 F4.2 pc e_r ? Adopted distance uncertainty 48 A1 --- n_r [a] Weighted mean of trigonometric and photometric distance
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 2 A2 --- --- [WD] 4- 11 A8 --- WD WD designation (HHMM+DDM, B1950) (1) 13- 27 A15 --- OName Other name 29- 34 A6 --- SpType Spectral type 36- 40 F5.2 pc r.tr ?=- Trigonometric distance 42- 45 F4.2 pc e_r.tr ?=- r.tr uncertainty 47- 51 F5.2 pc r.ph Photometric distance 53- 56 F4.2 pc e_r.ph ?=- r.ph uncertainty 58- 62 A5 --- Ref reference(s) number; see refs.dat file 64- 69 F6.3 mag Vmag ?=- Visual magnitude 70 A1 --- u_Vmag Uncertainty flag on Vmag 72- 74 A3 --- Notes [a-c, ] Note(s) (2)
Note (1): WD 0816+387 is the correct name of WD 0827+387 (in original paper) WD 1339-340 PM J13420-3415 are the correct names for WD 1339+259 PM J134020-3415 (in original table). Note (2): Notes as follows: a = Double degenerate; b = binary; c = photometric distances estimated in this paper.
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 2 I2 --- Ref Reference number 4- 22 A19 --- BibCode Bibcode 24- 49 A26 --- Aut Author's name(s) 51-146 A96 --- Com Comments
History: From electronic version of the journal
(End) Emmanuelle Perret [CDS] 29-Jun-2010
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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