Table 4
Final fate of IMBHs at redshift z = 0.
| Model A | |||||
|---|---|---|---|---|---|
| Form. | Clu. | N. Rec. (%) | GW Kick (%) | Evap. (%) | Ret. (%) |
| YCs | 14.2 | 74.0 | 11.8 | – | |
| S | GCs | 4.1 | 61.5 | 0.6 | 33.8 |
| NSCs | 1.8 | 39.5 | 0.5 | 58.2 | |
| H | NSCs | 0.8 | 85.6 | – | 13.6 |
| Model B | |||||
| Form. | Clu. | N. Rec. (%) | GW Kick (%) | Evap. (%) | Ret. (%) |
| YCs | 21.0 | 61.6 | 17.4 | – | |
| S | GCs | 0.8 | 34.3 | 0.5 | 64.4 |
| NSCs | 0.3 | 11.0 | 0.1 | 88.5 | |
| H | NSCs | 1.0 | 84.7 | – | 14.4 |
Notes. IMBHs are divided by formation channel (Column 1) and cluster type (Column 2). They can be expelled in our simulations as a result of a strong Newtonian recoil (Column 3), a post-merger relativistic kick (Column 4), or the evaporation of their host cluster (Column 5). The fraction of IMBHs that are retained within their hosts at z = 0 is presented in Column 6.
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