The white dwarf binary pathways survey – XI. The Gaia - GALEX UV excess sample for systems within 350 pc
9 affiliations
- 1Astrophysics Research Cluster, School of Mathematical and Physical Sciences, University of Sheffield , Sheffield S3 7RH ,
- 2Department of Physics, Università degli Studi di Trieste , Via A. Valerio 2, I-34127 Trieste ,
- 3Department of Physics, University of Warwick , Coventry CV4 7AL ,
- 4Hamburger Sternwarte, University of Hamburg , Gojenbergsweg 112, D-21029 Hamburg ,
- 5Departamento de Física, Universidad Técnica Federico Santa María , Avenida España 1680, Valparaíso ,
- 6Departament de Física, Universitat Politècnica de Catalunya , c/Esteve Terrades 5, E-08860 Castelldefels ,
- 7Institut d’Estudis Espacials de Catalunya (IEEC) , C/Esteve Terradas, 1, Edifici RDIT, E-08860 Castelldefels ,
- 8Key Laboratory of Space Astronomy and Technology, National Astronomical Observatories, Chinese Academy of Sciences , Beijing 100101 ,
- 9Instituto de Física y Astronomía, Universidad de Valparaíso , Av. Gran Bretaña 1111, Valparaíso ,
Abstract
White dwarfs (WDs) with F-, G-, or K-type binary companions are the last common ancestor to a zoo of exotic phenomena. Finding a clean sample of such systems is difficult, as WDs in such binaries are usually outshone at optical wavelengths by their non-degenerate companion. It is useful to have a sample of such binaries; they can be studied to investigate binary evolution, as they may have undergone a previous phase of mass transfer. Using Gaia data release 3 and GALEX, we compile a sample of 2597 candidate WD + FGK systems within 350 pc. These were identified via their ultraviolet excesses relative to MESA Isochrones and Stellar Tracks model predictions consistent with the Gaia parameters of their non-degenerate companions. We estimate the mass, surface gravity, and effective temperature of the WDs by fitting the excess ultraviolet flux to models, or through interpolation where only one ultraviolet band was available. We also estimate the age of the system where possible, by comparing against any wide WD companions in higher-order stellar systems, or by checking if the system is a member of a cluster. On comparing against Simbad, we estimate the level of contamination within our sample to be between 10 per cent and 35 per cent. This is a valuable sample for investigating WD + FGK binaries, particularly those containing hotter WDs (Teff, WD ≳ 25 kK), and systems with post-main-sequence companions.
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BibTeX
@article{garbutt2026white,
title = {{The white dwarf binary pathways survey – XI. The Gaia - GALEX UV excess sample for systems within 350 pc}},
author = {James A Garbutt and S G Parsons and N Gentile Fusillo and B T Gänsicke and M S Hernandez and F Lagos-Vilches and R Raddi and A Rebassa-Mansergas and J J Ren and M R Schreiber and O Toloza and M Zorotovic},
journal = {Monthly Notices of the Royal Astronomical Society},
year = {2026},
month = oct,
doi = {10.1093/mnras/stag1766},
url = {https://academic.oup.com/mnras/article/doi/10.1093/mnras/stag1766/8962097},
note = {CC BY 4.0},
}
RIS
TY - JOUR
TI - The white dwarf binary pathways survey – XI. The Gaia - GALEX UV excess sample for systems within 350 pc
AU - James A Garbutt
AU - S G Parsons
AU - N Gentile Fusillo
AU - B T Gänsicke
AU - M S Hernandez
AU - F Lagos-Vilches
AU - R Raddi
AU - A Rebassa-Mansergas
AU - J J Ren
AU - M R Schreiber
AU - O Toloza
AU - M Zorotovic
PY - 2026
DA - 2026/10/21
JO - Monthly Notices of the Royal Astronomical Society
DO - 10.1093/mnras/stag1766
UR - https://academic.oup.com/mnras/article/doi/10.1093/mnras/stag1766/8962097
AB - White dwarfs (WDs) with F-, G-, or K-type binary companions are the last common ancestor to a zoo of exotic phenomena. Finding a clean sample of such systems is difficult, as WDs in such binaries are usually outshone at optical wavelengths by their non-degenerate companion. It is useful to have a sample of such binaries; they can be studied to investigate binary evolution, as they may have undergone a previous phase of mass transfer. Using Gaia data release 3 and GALEX, we compile a sample of 2597 candidate WD + FGK systems within 350 pc. These were identified via their ultraviolet excesses relative to MESA Isochrones and Stellar Tracks model predictions consistent with the Gaia parameters of their non-degenerate companions. We estimate the mass, surface gravity, and effective temperature of the WDs by fitting the excess ultraviolet flux to models, or through interpolation where only one ultraviolet band was available. We also estimate the age of the system where possible, by comparing against any wide WD companions in higher-order stellar systems, or by checking if the system is a member of a cluster. On comparing against Simbad, we estimate the level of contamination within our sample to be between 10 per cent and 35 per cent. This is a valuable sample for investigating WD + FGK binaries, particularly those containing hotter WDs (T_eff, WD ≳ 25 kK), and systems with post-main-sequence companions.
SN - 0035-8711
SN - 1365-2966
ER -