  Discovery and characterisation of black holes (BHs), neutron stars (NSs), and
white dwarfs (WDs) with detached luminous companions (LCs) in wide orbits are
exciting because they are important test beds for dark remnant (DR) formation
physics as well as binary stellar evolution models. Recently, 187 candidates
have been identified from Gaia's non-single star catalog as wide orbit
(P_orb/days>45), detached binaries hosting DRs. We identify UV counterparts for
49 of these sources in the archival GALEX data. Modeling the observed spectral
energy distribution (SED) spanning FUV-NUV to IR for these sources and stellar
evolution models, we constrain the LC properties including mass, bolometric
luminosity, and effective temperature for these 49 sources. Using the LC
masses, and the astrometric mass function constrained by Gaia, we constrain the
DR masses for these sources. We find that 9 have masses clearly in the NS or BH
mass range. Fifteen sources exhibit significant NUV excess and 4 show excess
both in FUV and NUV. The simplest explanation for these excess UV fluxes is
that the DRs in these sources are WDs. Using SED modeling we constrain the
effective temperature and bolometric luminosity for these 15 sources. Our
estimated DR masses for all of these 15 sources are lower than the
Chandrasekhar mass limit for WDs. Interestingly, five of these sources had been
wrongly identified as neutron stars in literature.
