  Identification of white dwarfs (WD) with main-sequence (MS) companions and
characterization of their properties can put important constraints on our
understanding of binary stellar evolution and guide the theoretical predictions
for a wide range of interesting transient events relevant for, e.g., Rubin
Observatory (LSST), ZTF, and LISA. In this study, we combine ultraviolet (UV)
and optical color-magnitude diagrams (CMDs) to identify unresolved WD--MS
binaries. In particular, we combine high-precision astrometric and photometric
data in the optical from \gaia\ -DR3 and UV data from GALEX GR6/7 to identify
93 WD--MS candidates within 100 pc. Of these, 80 are newly identified. Using
the Virtual Observatory SED Analyzer (VOSA) we fit the spectral energy
distributions (SEDs) of all our candidates and derive stellar parameters, such
as effective temperature, bolometric luminosity, and radius for both
companions. We find that our identification method helps identify hotter and
smaller WD companions (majority with $\geq$10,000 K and $\leq$0.02 $R_\odot$)
relative to the WDs identified by past surveys. We infer that these WDs are
relatively more massive (median $\sim$ $0.76\,M_\odot$). We find that most of
the MS companions in our binaries are of the $K$ and $M$ spectral types.
