J/A+A/699/A153 Gaia DR3 WD-MS parameters (Rebassa-Mansergas+, 2025)
Magnitude-limited catalogue of unresolved white dwarf-main sequence binaries
from Gaia DR3.
Rebassa-Mansergas A., Solano E., Brown A.J., Parsons S.G.,
Murillo-Ojeda R., Raddi R., Camisassa M., Torres S., van Roestel J.
<Astron. Astrophys. 699, A153 (2025)>
=2025A&A...699A.153R 2025A&A...699A.153R (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, spectroscopic ; Binaries, eclipsing ;
Stars, white dwarf ; Effective temperatures ;
Parallaxes, trigonometric ; Photometry ; Optical
Keywords: binaries: close - stars: late-type - white dwarfs
Abstract:
Binary stars containing a white dwarf and a main-sequence star, WDMS
binaries, can be used to study a wide range of aspects of stellar
astrophysics. We build a magnitude-limited sample of unresolved WDMS
binaries from Gaia DR3 to enlarge these studies. We look for WDMS with
available spectra whose location in the Gaia colour-magnitude diagram
bridges between the evolutionary sequences of single white dwarfs and
the main-sequence. To exclude spurious sources we apply quality cuts
on the Gaia photometry and astrometry and we fit the SED (spectral
energy distribution) of the objects with VOSA (Virtual Observatory SED
Analyser) to exclude single sources. We further clean the sample via
visual inspection of the Gaia spectra and publicly available images of
the objects. We re-fit the SEDs of the finally selected WDMS with VOSA
using composite models to measure their stellar parameters and we
search for eclipsing systems by inspecting available ZTF and CRTS
light curves. The catalogue consists of 1312 WDMS and we manage to
derive stellar parameters for 435. This is because most WDMS are
dominated by the main-sequence companions, making it hard to derive
parameters for the white dwarfs. We also identify 67 eclipsing systems
and estimate a lower limit to the completeness of the sample to be
∼50% (∼5% if we consider that not all WDMS in the studied region have
Gaia spectra). Our catalogue increases by one order of magnitude the
volume-limited sample we presented in our previous work. Despite the
fact that the sample is incomplete and suffers from heavy
observational biases, it is well characterised and can therefore be
used to further constrain binary evolution by comparing the observed
properties to those from synthetic samples obtained modeling the WDMS
population in the Galaxy, taking into account all selection effects.
Description:
Gaia DR3 IDs, coordinates, parallaxes and photometry together with the
stellar parameters (white dwarf temperatures, surface gravities and
masses and main sequence star temperatures), periods (when available
from the eclipses) and notes for 1312 WDMS unresolved binaries from
Gaia DR3.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 115 1312 Parameters for the 1312 Gaia DR3 WDMS
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See also:
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 19 I19 --- GaiaDR3 Gaia DR3 ID
21- 29 F9.5 deg RAdeg Right ascension (ICRS) at Ep=2016.0
31- 39 F9.5 deg DEdeg Declination (ICRS) at Ep=2016.0
41- 45 F5.2 mas plx Parallax
47- 51 F5.2 mag Gmag Gaia G magnitude
53- 57 F5.2 mag Bpmag Gaia Bp magnitude
59- 63 F5.2 mag Rpmag Gaia Rp magnitude
65- 69 I5 K TeffWD ?=0 WD effective temperature
71- 74 I4 K e_TeffWD ?=0 WD effective temperature error
76- 79 F4.2 [cm/s2] loggWD ?=0 WD surface gravity
81- 84 F4.2 [cm/s2] e_loggWD ?=0 WD surface gravity error
86- 89 F4.2 Msun MassWD ?=0 WD mass
91- 94 F4.2 Msun e_MassWD ?=0 WD mass error
96- 99 I4 K TeffMS ?=0 MS effective temperature
101-102 I2 K e_TeffMS ?=0 MS effective temperature error
104-110 F7.5 d Per ?=0 Orbital period
112-113 I2 --- Ref ?=0 Reference for the eclipsing system (1)
115 I1 --- cont [0/1] If 1, possibly contaminated by companion
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Note (1): References as follows:
0 = This work
1 = Brown et al. (2023MNRAS.521.1880B 2023MNRAS.521.1880B)
2 = Bruch & Diaz (1998AJ....116..908B 1998AJ....116..908B)
3 = Chen et al. (2020ApJS..249...18C 2020ApJS..249...18C, Cat. J/ApJS/249/18)
4 = Kosakowski et al. (2022MNRAS.516..720K 2022MNRAS.516..720K)
5 = Mowlavi et al. (2023A&A...674A..16M 2023A&A...674A..16M, Cat. I/358)
6 = Nebot Gomez-Moran et al. (2009A&A...495..561N 2009A&A...495..561N)
7 = O'Donoghue et al. (2003MNRAS.345..506O 2003MNRAS.345..506O)
8 = Parsons et al. (2013MNRAS.429..256P 2013MNRAS.429..256P)
9 = Parsons et al. (2025MNRAS.537.2112P 2025MNRAS.537.2112P)
10 = Priyatikanto et al. (2022MNRAS.516.1183P 2022MNRAS.516.1183P)
11 = Pyrzas et al. (2009MNRAS.394..978P 2009MNRAS.394..978P)
12 = Pyrzas et al. (2012MNRAS.419..817P 2012MNRAS.419..817P)
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Acknowledgements:
Alberto Rebassa-Mansergas, alberto.rebassa(at)upc.edu
(End) A. Rebassa-Mansergas [UPC, Spain], P. Vannier [CDS] 20-May-2025