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Intermediate-mass black holes (IMBHs) may provide the missing link tounderstanding the growth of supermassive black holes in the early Universe.Some formation scenarios predict that IMBHs could have formed by runawaycollisions in globular clusters (GCs). Understanding the influence of an IMBHin the center of a GC on its environment might provide indirect detectionmethods. Our goal is to test the effects of different initial compositions ofGCs on their evolution in a tidal field. We pin down the crucial observablesthat indicate the presence of an IMBH at the center of the cluster. In additionto central IMBHs, we also consider the effects of different stellar-mass blackhole retention and stellar binary fractions. We performed a set of 22 N-bodysimulations and varied particle numbers, IMBH masses, stellar-mass black-holeretention fractions, and stellar binary fractions. These models are all run inan external tidal field to study the effect of black holes on the cluster massloss, mass function, and life times. Finally, we compared our results withobservational data. We found that a central massive black hole increases theescape rate of high-mass stars from a star cluster, implying that the relativedepletion of the mass function at the low-mass end proceeds less rapidly.Furthermore, we found a similar behavior for a cluster hosting a high number ofstellar-mass black holes instead of one massive central IMBH. The presence ofan IMBH also weakly affects the fraction of the cluster mass that isconstituted by stellar remnants, as does the presence of primordial binaries.We compared our simulations with observational data from the literature andfound good agreement between our models and observed mass functions andstructural parameters of GCs. We exploited this agreement to identify GCs thatcould potentially host IMBHs.

N-body simulations of globular clusters in tidal fields: Effects of intermediate-mass black holes