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In this paper, we address the question: What is the probability ofstellar-mass black hole (BH) binaries co-existing in a globular cluster with anintermediate-mass black hole (IMBH)? Our results suggest that the detection ofone or more BH binaries can strongly constrain the presence of an IMBH in mostGalactic globular clusters. More specifically, the detection of one or more BHbinaries could strongly indicate against the presence of an IMBH more massivethan $\gtrsim 10^3$ M$_{\rm \odot}$ in roughly 80\% of the clusters in oursample. To illustrate this, we use a combination of N-body simulations andanalytic methods to weigh the rate of formation of BH binaries against theirejection and/or disruption rate via strong gravitational interactions with thecentral (most) massive BH.  The eventual fate of a sub-population of stellar-mass BHs (with or withoutbinary companions) is for all BHs to be ejected from the cluster by the centralIMBH, leaving only the most massive stellar-mass BH behind to form a closebinary with the IMBH. During each phase of evolution, we discuss the rate ofinspiral of the central BH-BH pair as a function of both the properties of thebinary and its host cluster.

On the coexistence of stellar-mass and intermediate-mass black holes in globular clusters