Towards a volumetric census of close white dwarf binaries I.Reference samples

TL;DR

This paper aims to create a comprehensive, volume-limited catalog of close white dwarf binaries within 300 parsecs to serve as a benchmark for understanding their evolution and population statistics.

Contribution

It assembles and vetts reference samples of white dwarf binaries within 300 pc, covering key sub-classes, to establish a representative, statistically sound dataset for future studies.

Findings

Compiled a 'Gold' Sample of white dwarf binaries within 300 pc.

Analyzed differences between magnitude and volume limited samples.

Discussed evolutionary pathways and observational properties across the Gaia HR diagram.

Abstract

Close white dwarf binaries play an important role across a range of astrophysics, including thermonuclear supernovae, the Galactic low-frequency gravitational wave signal, and the chemical evolution of the Galaxy. Progress in developing a detailed understanding of the complex, multi-threaded evolutionary pathways of these systems is limited by the lack of statistically sound observational constraints on the relative fractions of various sub-populations, and their physical properties. The available samples are small, heterogeneous, and subject to a multitude of observational biases. Our overarching goal is to establish a volume-limited sample of all types of white dwarf binaries that is representative of the underlying population as well as sufficiently large to serve as a benchmark for future binary population models. In this first paper, we provide an overview of the project, and assemble reference samples within a distance limit of 300\,pc of known white dwarf binaries spanning the most common sub-classes: post-common envelope binaries containing a white dwarf plus a main sequence star, cataclysmic variables and double-degenerate binaries. We carefully vet the members of these "Gold" Samples, which span most of the evolutionary parameter space of close white dwarf binary evolution. We also explore the differences between magnitude and volume limited close white dwarf binary samples, and discuss how these systems evolve in their observational properties across the Gaia Hertzsprung-Russell diagram.