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Populations of stellar-mass black holes (BHs) in globular clusters (GCs)influence their dynamical evolution and have important implications on one ofthe main formation channels for gravitational wave sources. Inferring the sizeof these populations remains difficult, however. In this work, multimass modelsof 34 Milky Way GCs, first presented in Dickson et al., are used to explore thepresent-day BH populations of a large sample of clusters. Direct constraints onboth the total and visible mass components provided by several observablesallow these models to accurately determine the distribution of the dark mass(including BHs) within clusters, as we demonstrate in a proof-of-conceptfitting of the models to mock observations extracted from Monte Carlo clustermodels. New constraints on the BH population retained to the present-day ineach cluster are inferred from our models. We find that BH mass fractionsranging from 0 to 1 per cent of the total mass are typically required toexplain the observations, except for Omega Cen, for which we infer a massfraction of 5 per cent, in agreement with previous works. Relationships betweenthe dark remnant populations and other cluster parameters are examined,demonstrating a clear anti-correlation between the amount of BHs and masssegregation between visible stars, as well as a correlation between remnantmass fractions and the dynamical age of clusters. Our inferred BH populationsare in good agreement overall with other recent studies using differentmethodologies, but with notable discrepancies for individual clusters.

Multimass modelling of Milky Way globular clusters -- II. present-day black hole populations