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Our knowledge of the birth mass function of neutron stars and black holes isbased on observations of binary systems but the binary evolution likely affectsthe final mass of the compact object. Gravitational microlensing allows us todetect and measure masses of isolated stellar remnants, which are nearlyimpossible to obtain with other techniques. Here, we analyze a sample of 4360gravitational microlensing events detected during the third phase of the OGLEsurvey. We select a subsample of 87 long-timescale low-blending events. Weestimate the masses of lensing objects by combining photometric data from OGLEand proper-motion information from OGLE and Gaia EDR3. We find 35high-probability dark lenses - white dwarfs, neutron stars, and black holes -which we use to constrain the mass function of isolated stellar remnants. Inthe range 1-100 M_Sun, occupied by neutron stars and black holes, the remnantmass function is continuous and can be approximated as a power-law with a slopeof $0.83^{+0.16}_{-0.18}$ with a tentative evidence against a broad gap betweenneutron stars and black holes. This slope is slightly flatter than the slope ofthe mass function of black holes detected by gravitational wave detectors LIGOand Virgo, although both values are consistent with each other within thequoted error bars. The measured slope of the remnant mass function agrees withpredictions of some population synthesis models of black hole formation.

Measuring the mass function of isolated stellar remnants with gravitational microlensing. II. Analysis of the OGLE-III data