Physical Properties of the Current Census of Northern White Dwarfs within 40 pc of the Sun

TL;DR

This paper provides a comprehensive analysis of white dwarfs within 40 parsecs of the Sun, expanding the census by 40%, analyzing their physical properties, and identifying new objects and characteristics through spectroscopic survey data.

Contribution

It presents an expanded and more complete census of nearby white dwarfs, including new discoveries and a homogeneous atmospheric analysis highlighting the prevalence of massive and cool white dwarfs.

Findings

178 white dwarfs within 40 pc, 40% increase in census

Large fraction of massive, cool, and old white dwarfs

Discovery of 2 new ZZ Ceti pulsators

Abstract

We present a detailed description of the physical properties of our current census of white dwarfs within 40 pc of the Sun, based on an exhaustive spectroscopic survey of northern hemisphere candidates from the SUPERBLINK proper motion database. Our method for selecting white dwarf candidates is based on a combination of theoretical color-magnitude relations and reduced proper motion diagrams. We reported in an earlier publication the discovery of nearly 200 new white dwarfs, and we present here the discovery of an additional 133 new white dwarfs, among which we identify 96 DA, 3 DB, 24 DC, 3 DQ, and 7 DZ stars. We further identify 178 white dwarfs that lie within 40 pc of the Sun, representing a 40% increase of the current census, which now includes 492 objects. We estimate the completeness of our survey at between 66 and 78%, allowing for uncertainties in the distance estimates. We also perform a homogeneous model atmosphere analysis of this 40 pc sample and find a large fraction of massive white dwarfs, indicating that we are successfully recovering the more massive, and less luminous objects often missed in other surveys. We also show that the 40 pc sample is dominated by cool and old white dwarfs, which populate the faint end of the luminosity function, although trigonometric parallaxes will be needed to shape this part of the luminosity function more accurately. Finally, we identify 4 probable members of the 20 pc sample, 4 suspected double degenerate binaries, and we also report the discovery of two new ZZ Ceti pulsators.