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

Leigh, Nathan W. C.; Luetzgendorf, Nora; Geller, Aaron M.; Maccarone, Thomas J.; Heinke, Craig O.; Sesana, Alberto

doi:10.1093/mnras/stu1437

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

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Sesana, Alberto
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Citation

Leigh, N. W. C., Luetzgendorf, N., Geller, A. M., Maccarone, T. J., Heinke, C. O., & Sesana, A. (2014). On the coexistence of stellar-mass and intermediate-mass black holes in globular clusters. Monthly Notices of the Royal Astronomical Society, 444 (1), 29-42. doi:10.1093/mnras/stu1437.

Cite as: https://hdl.handle.net/11858/00-001M-0000-0024-510D-4

Abstract

In this paper, we address the question: What is the probability of stellar-mass black hole (BH) binaries co-existing in a globular cluster with an intermediate-mass black hole (IMBH)? Our results suggest that the detection of one or more BH binaries can strongly constrain the presence of an IMBH in most Galactic globular clusters. More specifically, the detection of one or more BH binaries could strongly indicate against the presence of an IMBH more massive than $\gtrsim 10^3$ M$_{\rm \odot}$ in roughly 80\% of the clusters in our sample. To illustrate this, we use a combination of N-body simulations and analytic methods to weigh the rate of formation of BH binaries against their ejection and/or disruption rate via strong gravitational interactions with the central (most) massive BH. The eventual fate of a sub-population of stellar-mass BHs (with or without binary companions) is for all BHs to be ejected from the cluster by the central IMBH, leaving only the most massive stellar-mass BH behind to form a close binary with the IMBH. During each phase of evolution, we discuss the rate of inspiral of the central BH-BH pair as a function of both the properties of the binary and its host cluster.