  Based on the astrometry and photometry in Gaia DR3, we identified new nearby
white dwarfs and validated those that had been missed from recent white dwarf
catalogues despite being previously documented. To ensure the reliability of
their astrometric solutions, we used a cut on just two parameters from Gaia
DR3: the amplitude of the image parameter determination goodness-of-fit and the
parallax-over-error ratio. In addition, we imposed photometric signal-to-noise
requirements to ensure the reliable identification of white dwarfs when using
the colour-magnitude diagram.
  We have identified nine previously unreported white dwarfs within the local
population of 50 pc, and validated 21 previously reported white dwarfs missing
from the GCWD21 (Gentile Fusillo et al. 2021) and other recent volume-limited
white dwarf samples. A few of these objects belong to the rare class of
ultra-cool white dwarfs. Four white dwarfs in our sample have an effective
temperature of $T_{eff}\leq4000$ K within the $1\sigma$ interval, and two of
them have an absolute magnitude of $M_G > 16.0$ mag. The identified white
dwarfs are predominantly located in crowded fields, such as near the Galactic
plane or in the foreground of the Large Magellanic Cloud. We also find that 19
of these white dwarfs have common proper motion companions with angular
separations ranging from $1.1''$ to $7.1''$ and brightness differences between
the components of up to 9.8 magnitudes. One of these systems is a triple system
consisting of a white dwarf and two K dwarfs, while another is a double white
dwarf system. We have identified 103 contaminants among the 2338
high-confidence white dwarfs in the 50 pc subsample of the GCWD21 and have
found that their astrometric solutions in Gaia DR3 are spurious, improving the
purity by 4.4%.
