Table 1.
Properties of the primary halo at redshift z = 0 for all the zoom-in simulations used in this study.
| Simulation | ℳh | ℳ⋆ | Number of GMCs | Number of clusters | Number of BBH mergers |
|---|---|---|---|---|---|
| [M⊙] | [M⊙] | ||||
| m11i | 7.8 × 1010 | 9.2 × 108 | 3.48 × 104 | 3.49 × 104 | 1 |
| m11q | 1.6 × 1011 | 6.1 × 108 | 1.73 × 104 | 3.90 × 104 | 0 |
| m11e | 1.7 × 1011 | 1.4 × 109 | 4.13 × 104 | 5.87 × 104 | 87 |
| m11h | 2.1 × 1011 | 3.6 × 109 | 1.09 × 105 | 1.21 × 105 | 280 |
| m11d | 3.2 × 1011 | 3.9 × 109 | 8.54 × 104 | 1.85 × 105 | 2208 |
| m12i | 1.2 × 1012 | 6.7 × 1010 | 8.52 × 105 | 4.05 × 106 | 12 438 |
Notes. ℳh is the total mass of gas, star, and DM contained in the sphere inside which the mean matter density is 200 times the mean matter density of the Universe. The galaxy stellar mass ℳ⋆ is calculated as 90% of the stellar mass within 20 kpc of the halo centre. The selection criterion of massive clusters Mcl ≥ 6 × 104 M⊙ is only applied at the epoch the cluster is formed. The number of BBH mergers indicated for m12i is a weighted approximation, as not all the massive clusters could be integrated with CMC (see Paper II, and Sect. 3.2).
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