Merger Rates of Intermediate-mass Black Hole Binaries in Nuclear Star Clusters

Repeated mergers of stellar-mass black holes in dense star clusters can produce intermediate-mass black holes (IMBHs). In particular, nuclear star clusters at the centers of galaxies have deep enough potential wells to retain most of the black hole (BH) merger products, in spite of the significant recoil kicks due to anisotropic emission of gravitational radiation. These events can be detected in gravitational waves, which represent an unprecedented opportunity to reveal IMBHs. In this paper, we analyze the statistical results of a wide range of numerical simulations, which encompass different cluster metallicities, initial BH seed masses, and initial BH spins, and we compute the merger rate of IMBH binaries. We find that merger rates are in the range 0.01-10 Gpc(-3) yr(-1) depending on IMBH masses. We also compute the number of multiband detections in ground-based and space-based observatories. Our model predicts that a few merger events per year should be detectable with LISA, DECIGO, Einstein Telescope (ET), and LIGO for IMBHs with masses less than or similar to 1000 M (circle dot), and a few tens of merger events per year with DECIGO, ET, and LIGO only.

Automated summary

Repeated mergers of stellar-mass black holes in dense star clusters can lead to the formation of intermediate-mass black holes. These events can be detected through gravitational waves, providing an opportunity to study intermediate-mass black holes. Through numerical simulations and statistical analysis, the merger rates under different conditions have been determined, and the number of detections in ground-based and space-based observatories has been computed.