J/MNRAS/480/4505 A white dwarf catalogue from Gaia-DR2 (Jimenez-Esteban+, 2018)
A white dwarf catalogue from Gaia-DR2 and the Virtual Observatory.
Jimenez-Esteban F.M., Torres S., Rebassa-Mansergas A., Skorobogatov G.,
Solano E., Cantero C., Rodrigo C.
<Mon. Not. R. Astron. Soc., 480, 4505-4518 (2018)>
=2018MNRAS.480.4505J 2018MNRAS.480.4505J (SIMBAD/NED BibCode)
ADC_Keywords: Stars, white dwarf ; Stars, distances ; Effective temperatures ;
Stars, masses ; Stars, diameters
Keywords: astronomical data bases: miscellaneous - catalogues -
virtual observatory tools - stars: evolution - (stars:) white dwarfs -
Galaxy: stellar content
Abstract:
We present a catalogue of 73221 white dwarf candidates extracted from
the astrometric and photometric data of the recently published
Gaia-DR2 catalogue. White dwarfs were selected from the Gaia
Hertzsprung-Russell diagram with the aid of the most updated
population synthesis simulator. Our analysis shows that Gaia has
virtually identified all white dwarfs within 100pc from the Sun.
Hence, our sub-population of 8555 white dwarfs within this distance
limit and the colour range considered, -0.52<(GBP-GRP)<0.80, is
the largest and most complete volume-limited sample of such objects to
date. From this sub-sample, we identified 8343 CO-core and 212
ONe-core white dwarf candidates and derived a white dwarf space
density of 4.9±0.4x10-3pc-3. A bifurcation in the
Hertzsprung-Russell diagram for these sources, which our models do not
predict, is clearly visible. We used the Virtual Observatory SED
Analyzer tool to derive effective temperatures and luminosities for
our sources by fitting their spectral energy distributions, that we
built from the ultraviolet to the near-infrared using publicly
available photometry through the Virtual Observatory. From these
parameters, we derived the white dwarf radii. Interpolating the radii
and effective temperatures in hydrogen-rich white dwarf cooling
sequences, we derived the surface gravities and masses. The Gaia 100pc
white dwarf population is clearly dominated by cool (∼8000K)
objects and reveals a significant population of massive
(M∼0.8M☉) white dwarfs, of which no more than ∼30-40 per cent
can be attributed to hydrogen-deficient atmospheres, and whose origin
remains uncertain.
Description:
With the aid of a detailed Monte Carlo simulator we built a thorough
population synthesis model of the thin disc, thick disc, and halo
white dwarf population of our Galaxy. Our synthetic models incorporate
updated evolutionary sequences for both CO-core and ONe-core white
dwarfs, as well as hydrogen-rich and hydrogen-deficient atmospheres.
Additionally, we included in our models a complete treatment of the
different selection criteria and photometric and astrometric errors
predicted by Gaia performances. This permitted us to define the
regions within the Gaia HR diagram where we expected to identify white
dwarfs, as well as to predict its completeness and to estimate its
possible contamination.
We followed the recommendations given by Evans et al.
(2018A&A...616A...4E 2018A&A...616A...4E) and Lindegren et al. (2018A&A...616A...2L 2018A&A...616A...2L), to
search for white dwarf candidates in the Gaia-DR2 catalogue with
accurate Gaia parallax and photometry. After adopting the photometric
criteria and colour limit, our query returned 73221 Gaia-DR2
counterparts, 72178 CO-core, and 1043 ONe-core white dwarf
candidates. They all form our catalogue of Gaia white dwarfs.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea.dat 370 73221 White dwarfs from Gaia-DR2 and the VO
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
Byte-by-byte Description of file: tablea.dat
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Bytes Format Units Label Explanations
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1- 23 F23.19 deg RAdeg Right ascension (ICRS) at Ep=2015.5
25- 48 F24.20 deg DEdeg Declination (ICRS) at Ep=2015.5
50- 68 I19 --- GaiaDR2 Gaia DR2 identifier
70- 89 F20.16 mas plx Parallax
91-109 F19.15 pc Dist Distance
111-136 F26.20 mas/yr pmRA Proper motion in right ascension
138-164 F27.21 mas/yr pmDE Proper motion in declination
166-175 F10.7 mag Gmag G-band mean magnitude
177-186 F10.7 mag BPmag Integrated BP mean magnitude
188-197 F10.7 mag RPmag Integrated RP mean magnitude
199-203 I5 K Teff ? Effective temperature from SED fitting (1)
205-208 F4.2 [cm/s2] loggVOSA ? Surface gravity from SED fitting (1)
210-223 F14.12 Lsun Lbol ? Bolometric luminosity of the object (1)
225-228 F4.2 [cm/s2] logg ? Surface gravity from the evolutionary
sequences
230-234 F5.3 [cm/s2] e_logg ? Error on logg
236-242 F7.5 Rsun Rad ? Radius obtained from the effective
temperature and luminosity
244-250 F7.5 Rsun e_Rad ? Error on Rad
252-257 F6.4 Msun M ? Mass obtained from the evolutionary
sequences
259-264 F6.4 Msun e_M ? Error on M
266-296 A31 --- Sname Simbad name
298-312 A15 --- Stype Simbad type
314-356 A43 --- Sotype Simbad other type
358-370 A13 --- SSptype Simbad spectral type
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Note (1): VOSA (Bayo et al. 2008A&A...492..277B 2008A&A...492..277B) is a VO tool designed to
determine physical parameters (such as effective temperature and
luminosity) of thousands of objects at once.
VOSA compares observed photometry, gathered from a significant number
of VO complaint catalogues, to different collections of theoretical
models.
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 30-May-2022