The black hole retention fraction in star clusters

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Table 1.

Parameters of the star-cluster models used in this paper.

N (M_tot(M_⊙))	r_v (pc)	t_rh (Myr)	t_cr (Myr)	t_end (Myr)
1k	0.5	6.1	0.61	65
(5 × 10²)	1.0	19	1.9	201
	2.0	49	4.9	523
3k	0.5	9.3	0.36	38
(1.6 × 10³)	1.0	27	1.0	110
	2.0	75	3.0	313
10k	0.5	15	0.20	35
(5.5 × 10³)	1.0	42	0.56	99
	2.0	118	1.6	280
25k	0.5	21	0.13	23
(1.4 × 10⁴)	1.0	60	0.36	64
	2.0	168	1.0	179
50k	0.5	28	0.088	16
(2.8 × 10⁴)	1.0	79	0.25	45
	2.0	223	0.71	125
100k	0.5	37	0.062	17
(5.6 × 10⁴)	1.0	107	0.18	43
	2.0	301	0.50	119

Notes. For each number of stars (with an approximate total mass), there are the initial virial radius, half-mass relaxation time, crossing time, and the approximate time up to which we followed the integration. The estimated time of formation of the last BH in our models is ≈11.7 Myr.

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