  We created the APOGEE-GALEX-\emph{Gaia} catalog to study white dwarfs
binaries. This database aims to create a minimally biased sample of WD binary
systems identified from a combination of GALEX, {\it Gaia}, and APOGEE data to
increase the number of WD binaries with orbital parameters and chemical
compositions. We identify 3,414 sources as WD binary candidates, with
nondegenerate companions of spectral types between F and M, including main
sequence, main sequence binaries, subgiants, sub-subgiants, red giants, and red
clump stars. Among our findings are (a) a total of 1,806 systems having
inferred WD radii $R < 25$ R$_{\Earth}$, which constitute a more reliable group
of WD binary candidates within the main sample; (b) a difference in the
metallicity distribution function between WD binary candidates and the control
sample of most luminous giants ($M_H < -3.0$); (c) the existence of a
population of sub-subgiants with WD companions; (d) evidence for shorter
periods in binaries that contain WDs compared to those that do not, as shown by
the cumulative distributions of APOGEE radial velocity shifts; (e) evidence for
systemic orbital evolution in a sample of 252 WD binaries with orbital periods,
based on differences in the period distribution between systems with red clump,
main sequence binary, and sub-subgiant companions and systems with main
sequence or red giant companions; and (f) evidence for chemical enrichment
during common envelope (CE) evolution, shown by lower metallicities in wide WD
binary candidates ($P > 100$ days) compared to post-CE ($P < 100$ days) WD
binary candidates.
