Description
In the era of new large-scale surveys, the number of confirmed white dwarfs (WDs) has reached several hundred thousand. With such vast datasets, it has become increasingly feasible to derive more specialized samples for separate analyses from the general WD population. Krzesiński et al. (2009) focused on analysing and determining the luminosity function of only hot WDs (Teff >20,000 K), including both DA and non-DA types, based on ~1000 WDs sample derived from SDSS DR4. Since then, a wealth of new data has become available, including high-quality measurements from Gaia, which provides improved distance estimates derived from parallax. The number of highly probably or suspected WDs based on Gaia DR2 was in the order of ~500 000, about 45 000 of which are likely to be hot WDs. In this work, I examine whether it is possible to significantly improve upon previous studies and whether the inclusion of new objects leads to major changes in the resulting hot white dwarf luminosity function.
