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We present an analysis of the degree of energy equipartition in a sample of101 Monte Carlo numerical simulations of globular clusters (GCs) hosting eithera system of stellar-mass black holes (BHS), an intermediate-mass black hole(IMBH) or neither of them. For the first time, we systematically explore thesignatures that the presence of BHS or IMBHs produces on the degree of energyequipartition and if these signatures could be found in current observations.We show that a BHS can halt the evolution towards energy equipartition in thecluster centre. We also show that this effect grows stronger with the number ofstellar-mass black holes in the GC. The signatures introduced by IMBHs dependon how dominant their masses are to the GCs and for how long the IMBH hasco-evolved with its host GCs. IMBHs with a mass fraction below 2% of thecluster mass produce a similar dynamical effect to BHS, halting the energyequipartition evolution. IMBHs with a mass fraction larger than 2% can producean inversion of the observed mass-dependency of the velocity dispersion, wherethe velocity dispersion grows with mass. We compare our results withobservations of Galactic GCs and show that the observed range of the degree ofenergy equipartition in real clusters is consistent with that found in ouranalysis. In particular, we show that some Galactic GCs fall within theanomalous behaviour expected for systems hosting a BHS or an IMBH and arepromising candidates for further dynamical analysis.

Effects of massive central objects on the degree of energy equipartition of globular clusters