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White dwarfs with planetary remnants in the era of Gaia – I. Six emission line systems
N. P. Gentile Fusillo (European Southern Observatory), Christopher J. Manser (University of Warwick), Boris T. Gänsicke (University of Warwick), Odette Toloza (University of Warwick), D. Koester (Christian-Albrechts-Universität zu Kiel), Erik Dennihy (International Gemini Observatory), Warren R. Brown (Center for Astrophysics Harvard & Smithsonian), Jay Farihi (University College London), Mark Hollands (University of Warwick), Matthew John Hoskin (University of Warwick), Paula Izquierdo (Universidad de La Laguna, Instituto de Astrofísica de Canarias), T. M. Kinnear (University of Kent), Thomas R. Marsh (University of Warwick), Alejandro Santamaría-Miranda (European Southern Observatory), Anna Francesca Pala (European Southern Observatory), Seth Redfield (Wesleyan University), P. Rodríguez-Gil (Universidad de La Laguna, Instituto de Astrofísica de Canarias), Matthias R. Schreiber (Millenium Nucleus for Planet Formation, Universidad Técnica Federico Santa María), Dimitri Veras (University of Warwick), David J. Wilson (McDonald Observatory, The University of Texas at Austin)
Résumé : ABSTRACT White dwarfs with emission lines from gaseous debris discs are among the rarest examples of planetary remnant hosts, but at the same time they are key objects for studying the final evolutionary stage of planetary systems. Making use of the large number of white dwarfs identified in Gaia Data Release 2 (DR2), we are conducting a survey of planetary remnants and here we present the first results of our search: six white dwarfs with gaseous debris discs. This first publication focuses on the main observational properties of these objects and highlights their most unique features. Three systems in particular stand out: WD J084602.47+570328.64 displays an exceptionally strong infrared excess that defies the standard model of a geometrically thin, optically thick dusty debris disc; WD J213350.72+242805.93 is the hottest gaseous debris disc host known with $\mbox{$T_{\mathrm{eff}}$}=29\,282$ K; and WD J052914.32–340108.11 in which we identify a record number of 51 emission lines from five elements. These discoveries shed light on the underlying diversity in gaseous debris disc systems and bring the total number of these objects to 21. With these numbers we can now start looking at the properties of these systems as a class of objects rather than on a case-by-case basis.