Table A.4
The dynamical BHs: binary parameters.
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) |
| NAME | Spectral | Porb | K2 | f(M1) | M1 ∗ | q | i | vrotsini | Ref. |
| type | (h) | (km s-1) | ( M⊙) | ( M⊙) | (°) | (km s-1) | |||
|
|
|||||||||
| Swift J1357.2–0933† | M2−4V | 2.8 ± 0.3 | 967 ± 49 | 11 ± 2 | > 8.3 | ~0.04 | ~90 | Corral-Santana et al. (2013); Mata Sánchez et al. (2015) † | |
|
|
|||||||||
| XTE J1650–500 | ~K4V | 7.69 ± 0.02 | 435 ± 30 | 2.7 ± 0.6 | ≤ 7.3 | > 47 | Orosz et al. (2004) | ||
|
|
|||||||||
| XTE J1118+480 | K7–M1V | 4.078414 ± 0.000005 | 709 ± 1 | 6.27 ± 0.04 | 6.9−8.2 | 0.024 ± 0.009 | 68−79 |
|
Khargharia et al. (2013); Torres et al. (2004) |
| González Hernández et al. (2008b); Calvelo et al. (2009b) | |||||||||
|
|
|||||||||
| XTE J1859+226 | ~K5V | 6.58 ± 0.05 | 541 ± 70 | 4.5 ± 0.6 | >5.42 | <70 | Corral-Santana et al. (2011) | ||
| (V406 Vul) | |||||||||
|
|
|||||||||
| SAXJ1819.3-2525 | B9III | 67.6152 ± 0.0002 | 211 ± 3 | 2.7 ± 0.1 | 6.4 ± 0.6 | 0.63−0.70 | 72 ± 4 | 100.9 ± 0.8 | Orosz et al. (2001); MacDonald et al. (2014) |
| (V4641 Sgr) | |||||||||
|
|
|||||||||
| XTE J1550–564 | K2–4IV | 37.0088 ± 0.0001 | 363 ± 6 | 7.7 ± 0.4 | 7.81−15.6 | ≈ 0.03 | 75 ± 4 | 55 ± 5 | Orosz et al. (2002, 2011b) |
|
|
|||||||||
| GRO J1655–40 | F6IV | 62.920 ± 0.003 | 226.1 ± 0.8 | 2.73 ± 0.09 | 6.0 ± 0.4 | 0.42 ± 0.03 | 69 ± 2 |
|
Orosz & Bailyn (1997); van der Hooft et al. (1998); Shahbaz et al. (1999, 2003) |
| (N. Sco 94) | Beer & Podsiadlowski (2002); González Hernández et al. (2008a) | ||||||||
|
|
|||||||||
| GRS 1009-45 | K7–M0V | 6.8449 ± 0.0003 | 475 ± 6 | 3.2 ± 0.1 | ≳ 4.4 | 0.055 ± 0.010 | 37−80 | 87 ± 5 | Filippenko et al. (1999); Shahbaz et al. (1996); Macias et al. (2011) |
| (N. Vel 93) | |||||||||
|
|
|||||||||
| GRS 1915+105 | K1–5III | 812 ± 4 | 126 ± 1 | 7.0 ± 0.2 | 12 ± 2 | 0.042 ± 0.024 | 60 ± 5 | 21 ± 4 | Harlaftis & Greiner (2004); Steeghs et al. (2013) |
| (V406 Vul) | Reid et al. (2014) | ||||||||
|
|
|||||||||
| GRO J0422+32 | M4–5V | 5.09185 ± 0.000005 | 378 ± 16 | 1.19 ± 0.02 | 2−15 |
|
10−50 |
|
Webb et al. (2000); Casares et al. (1995b); Gelino & Harrison (2003) |
| Beekman et al. (1997); Harlaftis et al. (1999) | |||||||||
|
|
|||||||||
| GRS 1124-684 | K3–5V | 10.38254 ± 0.00007 | 407 ± 3 | 3.02 ± 0.06 | 3.8−7.5 | 0.079 ± 0.007 | 39−65 | 85 ± 3 | Orosz et al. (1996); Shahbaz et al. (1997); Gelino et al. (2001a) |
| (N. Mus 91) | Casares et al. (1997); Wu et al. (2015) | ||||||||
|
|
|||||||||
| GS 2023+338 | K3III | 155.311 ± 0.002 | 208.5 ± 0.7 | 6.08 ± 0.06 |
|
0.067 ± 0.005 |
|
39 ± 1 | Casares et al. (1992, 1993); Casares & Charles (1994); Casares (1996) |
| (V404 Cyg) | Wagner et al. (1992); Shahbaz et al. (1994); Khargharia et al. (2010) | ||||||||
|
|
|||||||||
| GS 2000+251 | K3–7V | 8.258095 ± 0.000005 | 520 ± 5 | 5.0 ± 0.1 | 5.5−8.8 | 0.04 ± 0.01 | 54−60 | 86 ± 8 | Charles et al. (1991); Casares et al. (1995a) |
| (QZ Vul) | Harlaftis et al. (1996); Ioannou et al. (2004) | ||||||||
|
|
|||||||||
| GS 1354-64 | G5III | 61.068 ± 0.002 | 279 ± 5 | 5.7 ± 0.3 | ≥ 7.6 ± 0.7 |
|
≤ 79 | 69 ± 8 | Casares et al. (2004, 2009) |
| (BW Cir) | |||||||||
|
|
|||||||||
| H 1705-250 | K3–M0V | 12.51 ± 0.03 | 448 ± 4 | 4.9 ± 0.1 | 4.9−7.9 | ≤ 0.053 | 48−80 | ≤ 79 | Remillard et al. (1996); Filippenko et al. (1997) |
| (N. Oph 77) | Harlaftis et al. (1997); Martin et al. (1995) | ||||||||
|
|
|||||||||
| 3A0620–003 | K2–7V | 7.7523372 ± 0.0000002 | 437 ± 2 | 2.79 ± 0.04 | 6.6 ± 0.3 | 0.074 ± 0.006 | 51.0 ± 0.9 | Cantrell et al. (2010); Orosz et al. (1994) | |
| González Hernández & Casares (2010) | |||||||||
|
|
|||||||||
| 1H J1659-487 | >GIV | 42.14 ± 0.01 | > 317 ± 10 | 5.8 ± 0.5 | > 6 | ≤ 0.125 | Hynes et al. (2003b, 2004); Muñoz-Darias et al. (2008) | ||
| (GX 339-4) | |||||||||
|
|
|||||||||
| 4U 1543–475 | A2V | 26.79377 ± 0.00007 | 124 ± 4 | 0.25 ± 0.01 | 8.4−10.4 | 0.25−0.31 | 20.7 ± 1.5 | 46 ± 2 | Orosz et al. (1998); Orosz (2003) |
| (IL Lup) | |||||||||
Notes. Columns: (1) Name of the dynamical black hole used hereafter; (2) spectral type of the companion star; (3) orbital period; (4) secondary star’s radial velocity amplitude; (5) mass function; (6) mass of the black hole; (7) binary mass ratio; (8) inclination of the system and (9) references.
The privileged values of M1 were assumed using Casares & Jonker (2014).
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