Table 1.
Comparison of the formation efficiencies per unit of star-forming mass of CBM: BH–BH, BH–NS, and NS–NS between the two models with different initial distributions: either Sana et al. (2012, old) or Moe & Di Stefano (2017, new).
| Metallicity merger typeb | Formation efficiency XCBM ( )a |
Relative MD17 / Sana | |
|---|---|---|---|
| Sana+12 (model M10) | MD17 (model I1) | ||
| Z = Z⊙ | |||
| NS-NS | 8.3 × 10−6 | 3.8 × 10−6 | 0.46 |
| BH-NSc | 9.0 × 10−8 | 1.1 × 10−7 | 1.22 |
| BH-BH | 3.5 × 10−7 | 1.5 × 10−7 | 0.43 |
| Z = 0.1 Z⊙ | |||
| NS-NS | 1.75 × 10−6 | 1.0 × 10−6 | 0.57 |
| BH-NS | 3.0 × 10−6 | 1.2 × 10−6 | 0.4 |
| BH-BH | 2.1 × 10−5 | 8.4 × 10−6 | 0.4 |
| Z = 0.01 Z⊙ | |||
| NS-NS | 1.7 × 10−6 | 1.2 × 10−6 | 0.71 |
| BH-NS | 9.6 × 10−7 | 3.6 × 10−7 | 0.38 |
| BH-BH | 5.3 × 10−5 | 2.9 × 10−5 | 0.55 |
Notes. The comparison is made at three different metallicities. No metallicity-dependence for the IMF is assumed here. We indicate in bold text the dominant metallicity (out of the three showed here) for the formation of each type of the double compact mergers.
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