While the original report emphasizes Roman's ability to detect dozens of isolated neutron stars via combined photometry and astrometry in the Galactic Bulge Time Domain Survey, simulations in the peer-reviewed Astronomy & Astrophysics study actually project that Roman could constrain the total galactic neutron star population at scales approaching millions when extrapolated across repeated epochs. The methodology relies on Milky Way population synthesis models calibrated against known pulsar distributions, without direct observational sample sizes beyond benchmark events; key limitations include assumptions about kick velocity distributions and the unknown fraction of neutron stars in the 2-5 solar mass range. This connects to earlier microlensing surveys by OGLE and MOA that detected compact-object candidates but lacked Roman's sub-milliarcsecond astrometric precision for direct mass measurements. A critical gap in initial coverage is the link to the neutron star-black hole mass gap: Roman data could statistically test whether a true desert exists between roughly 2 and 5 solar masses, informing supernova explosion models from events like GW170817. By measuring astrometric deflections rather than light curves alone, the telescope offers a pathway to map natal kicks exceeding 500 km/s, revealing how these remnants are ejected from star-forming regions and redistributed across the disk. This synthesis draws from the 2026 study, NASA's Roman reference mission design, and population synthesis work in ApJ on isolated compact objects.