A Gaia Data Release 2 catalogue of white dwarfs and a comparison with SDSS. Issue 4 (6th November 2018)

• Record Type: Journal Article
• Authors: Gentile Fusillo, Nicola Pietro; Tremblay, Pier-Emmanuel; Gänsicke, Boris T; Manser, Christopher J; Cunningham, Tim; Cukanovaite, Elena; Hollands, Mark; Marsh, Thomas; Raddi, Roberto; Jordan, Stefan; Toonen, Silvia; Geier, Stephan; Barstow, Martin; Cummings, Jeffrey D
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 482:Issue 4(2019)
• Page Start: 4570
• Page End: 4591
• Publication Date: 2018-11-06
• Subjects: catalogues -- surveys -- white dwarfs; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/sty3016
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We present a catalogue of white dwarf candidates selected from the second data release of Gaia (DR2). We used a sample of spectroscopically confirmed white dwarfs from the Sloan Digital Sky Survey (SDSS) to map the entire space spanned by these objects in the Gaia Hertzsprung–Russell diagram. We then defined a set of cuts in absolute magnitude, colour, and a number of Gaia quality flags to remove the majority of contaminating objects. Finally, we adopt a method analogous to the one presented in our earlier SDSS photometric catalogues to calculate a probability of being a white dwarf ( P WD ) for all Gaia sources that passed the initial selection. The final catalogue is composed of$486\, 641$ stars with calculated P WD from which it is possible to select a sample of${\simeq } 260\, 000$ high-confidence white dwarf candidates in the magnitude range 8 < G < 21. By comparing this catalogue with a sample of SDSS white dwarf candidates, we estimate an upper limit in completeness of 85 per cent for white dwarfs with G ≤ 20 mag and T eff >7000 K, at high Galactic latitudes (| b | > 20°). However, the completeness drops at low Galactic latitudes, and the magnitude limit of the catalogue varies significantly across the sky as a function of Gaia 's scanning law. We also provide the list of objects within our sample with available SDSS spectroscopy. We use this spectroscopic sample to characterize the observed structure of the white dwarf distribution in the H–R diagram.