Table 1
Fraction of systems per SN that result in double BHs that would merge in less than 13.8 Gyr (upper two rows) and aLIGO detection rates (lower two rows), assuming that all galaxies have the corresponding metallicity (Cols. 2–5) or are distributed according to our applied integrated metallicity distributions (last column “Integrated Z”).
| Metallicity −→ | Z⊙/ 50 | Z⊙/ 20 | Z⊙/ 10 | Z⊙/ 4 | Integrated Z |
|
|
|||||
| NBHBH/NSN below PISN gap | 6.7 × 10-4 | 1.3 × 10-3 | 3.4 × 10-4 | 0 | (0.69−13) × 10-5 |
| NBHBH/NSN above PISN gap | 2.7 × 10-4 | 0 | 0 | 0 | (0.011−1.8) × 10-5 |
|
|
|||||
| aLIGO rate (yr-1) below PISN gap | 3539 | 5151 | 501 | 0 | 19–550 |
| aLIGO rate (yr-1) above PISN gap | 5431 | 0 | 0 | 0 | 2.1–370 |
Notes. Here, the first number of the quoted range corresponds to our local approximation, the second to the global approximation, which form lower and upper limits (see text). Numbers are given for merging BH+BH binaries both below and above the PISN gap. The uncertainties in aLIGO detections rates are mainly caused by mapping the galactic metallicity distribution throughout the Universe (Sect. 4.3).
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