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With its exquisite astrometric precision, the latest Gaia data releaseincludes $\sim$$10^5$ astrometric binaries, each of which have measured orbitalperiods, eccentricities, and the Thiele-Innes orbital parameters. Using theseand an estimate of the luminous stars' masses, we derive the companion stars'masses, from which we identify a sample of 24 binaries in long period orbits($P_{\rm orb}\sim{\rm yrs}$) with a high probability of hosting a massive($>$1.4 $M_{\odot}$), dark companion: a neutron star (NS) or black hole (BH).The luminous stars in these binaries tend to be F-, G-, and K-dwarfs with thenotable exception of one hot subdwarf. Follow-up spectroscopy of eight of thesestars shows no evidence for contamination by white dwarfs or other luminousstars. The dark companions in these binaries span a mass range of 1.35-2.7$M_{\odot}$ and therefore likely includes both NSs and BHs without asignificant mass gap in between. Furthermore, the masses of several of theseobjects are $\simeq$1.7 $M_{\odot}$, similar to the mass of at least one of themerging compact objects in GW190425. Given that these orbits are too wide forsignificant mass accretion to have occurred, this sample implies that some NSsare born heavy ($\gtrsim$1.5 $M_{\odot}$). Additionally, the low orbitalvelocities ($\lesssim$20 km s$^{-1}$) of these binaries requires that at leastsome heavy NSs receive low natal kicks, otherwise they would have beendisrupted during core collapse. Although none will become gravitational wavesources within a Hubble time, these systems will be exceptionally useful fortesting binary evolution theory.

A Sample of Neutron Star and Black Hole Binaries Detected through Gaia DR3 Astrometry