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The search for intermediate-mass black holes (IMBHs) in the centre ofglobular clusters is often based on the observation of a central cusp in thesurface brightness profile and a rise towards the centre in the velocitydispersion profiles. Similar signatures, however, could result from othereffects, that need to be taken into account in order to determine the presence(or the absence) of an IMBH in these stellar systems. Following our previousexploration of the role of radial anisotropy in shaping these observationalsignatures, we analyse here the effects produced by the presence of apopulation of centrally concentrated stellar-mass black holes. We fit dynamicalmodels to omega Cen data, and we show that models with ~5% of their mass inblack holes (consistent with ~100% retention fraction after natal kicks) canreproduce the data. When simultaneously considering both radial anisotropy andmass segregation, the best-fit model includes a smaller population of remnants,and a less extreme degree of anisotropy with respect to the models that includeonly one of these features. These results underline that before conclusionsabout putative IMBHs can be made, the effects of stellar-mass black holes andradial anisotropy need to be properly accounted for.

The effect of stellar-mass black holes on the central kinematics of omega Cen: a cautionary tale for IMBH interpretations