Table 1
Formation efficiency (
) for Gaia BH3-like and BH-star systems obtained from different simulation models.
| Model | ηGaia BH3-like | ηGaia BH3-like (t > 10 Gyr) | ηGaia BH3-like (t > 10 Gyr) (vsys < 10 km s–1) | ηGaia BH3-like (t > 10 Gyr) (vsys < 1 km s–1) | ηBH-star (t > 10 Gyr) |
|---|---|---|---|---|---|
| fiducial | (9.7 ± 0.8) × 10–8 | (3.9 ± 0.5) × 10–8 | (2.8 ± 0.4) × 10–8 | (2.5 ± 0.4) × 10–8 | (1.6 ± 0.1) × 10–6 |
| fiducial2E8 | (1.0 ± 0.1) × 10–7 | (4.4 ± 0.2) × 10–8 | (3.5 ± 0.2) × 10–8 | (3.0 ± 0.2) × 10–8 | (1.6 ± 0.1) × 10–6 |
| ICthermal | (2.4 ± 0.1) × 10–7 | (1.0 ± 0.1) × 10–7 | (9.0 ± 0.8) × 10–8 | (7.8 ± 0.7) × 10–8 | (1.3 ± 0.1) × 10–6 |
| RLOp | (9.1 ± 0.8) × 10–8 | (3.5 ± 0.5) × 10–8 | (2.5 ± 0.4) × 10–8 | (2.3 ± 0.4) × 10–8 | (1.6 ± 0.1) × 10–6 |
| VK1 | (1.0 ± 0.1) × 10–7 | (3.9 ± 0.5) × 10–8 | (3.9 ± 0.5) × 10–8 | (8.5 ± 0.2) × 10–9 | (2.3 ± 0.1) × 10–6 |
| VK50 | (9.0 ± 0.8) × 10–8 | (4.0 ± 0.5) × 10–8 | 0 | 0 | (9.0 ± 0.3) × 10–7 |
| VK100 | (3.6 ± 0.5) × 10–8 | (1.1 ± 0.3) × 10–8 | 0 | 0 | (6.0 ± 0.2) × 10–7 |
| VK265 | (6.4 ± 2.1) × 10–9 | (2.1 ± 1.2) × 10–9 | 0 | 0 | (6.2 ± 0.2) × 10–8 |
| CEα3 | (9.7 ± 0.8) × 10–8 | (3.9 ± 0.5) × 10–8 | (2.8 ± 0.4) × 10–8 | (2.5 ± 0.4) × 10–8 | (2.5 ± 0.1) × 10–6 |
| CEα5 | (9.7 ± 0.8) × 10–8 | (3.9 ± 0.5) × 10–8 | (2.8 ± 0.4) × 10–8 | (2.5 ± 0.4) × 10–8 | (2.8 ± 0.1) × 10–6 |
| CEλXL10 | (9.7 ± 0.8) × 10–8 | (3.9 ± 0.5) × 10–8 | (2.8 ± 0.4) × 10–8 | (2.5 ± 0.4) × 10–8 | (1.4 ± 0.1) × 10–6 |
| CEλK21 | (9.7 ± 0.8) × 10–8 | (3.9 ± 0.5) × 10–8 | (2.8 ± 0.4) × 10–8 | (2.5 ± 0.4) × 10–8 | (1.4 ± 0.1) × 10–6 |
| Z1E-4 | (1.3 ± 0.1) × 10–7 | (4.8 ± 0.6) × 10–8 | (3.0 ± 0.5) × 10–8 | (2.7 ± 0.4) × 10–8 | (1.4 ± 0.1) × 10–6 |
| Z4E-4 | (1.1 ± 0.1) × 10–7 | (4.8 ± 0.6) × 10–8 | (2.1 ± 0.4) × 10–8 | (1.7 ± 0.3) × 10–8 | (1.4 ± 0.1) × 10–6 |
| Z8E-4 | (9.4 ± 0.8) × 10–8 | (3.9 ± 0.5) × 10–8 | (1.8 ± 0.4) × 10–8 | (1.4 ± 0.3) × 10–8 | (1.5 ± 0.1) × 10–6 |
| Z1E-3 | (9.2 ± 0.8) × 10–8 | (4.0 ± 0.5) × 10–8 | (2.1 ± 0.4) × 10–8 | (1.9 ± 0.4) × 10–8 | (1.6 ± 0.1) × 10–6 |
| Z4E-3 | (9.1 ± 0.8) × 10–8 | (5.3 ± 0.6) × 10–8 | (2.8 ± 0.5) × 10–8 | (2.1 ± 0.4) × 10–8 | (2.4 ± 0.1) × 10–6 |
| Z6E-3 | (9.4 ± 0.8) × 10–8 | (5.8 ± 0.6) × 10–8 | (3.9 ± 0.5) × 10–8 | (2.8 ± 0.4) × 10–8 | (2.7 ± 0.1) × 10–6 |
| Z8E-3 | (8.2 ± 0.8) × 10–8 | (6.2 ± 0.7) × 10–8 | (4.7 ± 0.6) × 10–8 | (3.3 ± 0.5) × 10–8 | (3.1 ± 0.1) × 10–6 |
| Z1E-2 | (8.2 ± 0.8) × 10–8 | (7.1 ± 0.7) × 10–8 | (7.0 ± 0.7) × 10–8 | (5.9 ± 0.6) × 10–8 | (3.4 ± 0.1) × 10–6 |
Notes. Column 1: model name; Column 2: formation efficiency of all Gaia BH3-like systems, as defined by the section cut (Sect. 3); Col. 3: same as Col. 2 but with the additional condition that the system is still in the BH-star configuration after 10 Gyr; Col. 4 (5): same as Col. 3 but with the additional condition that the binary has a systemic velocity of vsys < 10 km/s (vsys < 1 km/s); Col. 6: all BH-star systems with an age >10 Gyr. To calculate the formation efficiency, we assumed a 100% binary fraction. The errors are estimated as the square root of the counts over the total mass.
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