Merging stellar and intermediate-mass black holes in dense clusters: implications for LIGO, LISA, and the next generation of gravitational wave detectors

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Table 2.

Main results of N-body simulations.

ID	f_bnd	f_dis	f_IMRI	N_bbh	f_IMRI, ibh
					10² M_⊙	10³ M_⊙	10⁴ M_⊙	10⁵ M_⊙
S0	0.23	0.49	0.28	0	0.03	0.27	0.51	0.30
S1	0.17	0.61	0.22	2	0.03	0.27	0.38	0.16
S2	0.38	0.37	0.25	0	0.00	0.12	0.44	0.44
S3	0.26	0.42	0.32	2	0.04	0.48	0.44	0.31
S4	0.24	0.46	0.30	0	0.03	0.36	0.48	0.30
S5	0.26	0.31	0.42	22	0.21	0.29	0.31	0.46
S6	0.27	0.39	0.34	1	0.03	0.49	0.49	0.33

Notes. Column 1: set ID. Columns 2–4: fraction of models that remain bound, get disrupted, or form an IMRI. Column 5: number of mergers between stellar BHs. Columns 6–9: fraction of models forming an IMRI for different values of the IMBH mass.

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