Table B.1.
Spectral types and Teff of donor stars in BH LMXBs
| Object | Porb | Spect. Type | Method | Teff | References for |
|---|---|---|---|---|---|
| (d) | (°K) | Spect. Type | |||
| GRS 1915+105 | 33.85(16) | K1-5 III | NIR SPEC | 4241±219 | 1 |
| V404 Cyg | 6.471170(2) | G9-K1 III | VIS SPEC | 4570±110 | 2 |
| G8-K2 III | SED | 4570±219 | 3 | ||
| K2-4 III | NIR SPEC | 4242±110 | 4 | ||
| – | SPEC FIT | 4800±100 | 5 | ||
| – | – | 4544±48 | – | ||
| BW Cir | 2.54451(8) | G0-5 IV | VIS SPEC | 5589±201 | 6 |
| GX 339-4 | 1.7587(5) | K1-2 IV | NIR SPEC | 4756±60 | 7 |
| XTE J1550-564 | 1.5420333(24) | K2-4 IV | VIS SPEC | 4536±160 | 8 |
| MAXI J1820+070 | 0.68549(1) | K3-5 V | VIS SPEC | 4645±195 | 9 |
| N. Oph 77 | 0.5228(44) | K1-5 V | VIS SPEC | 4810±360 | 10 |
| K3-5 V a | VIS SPEC | 4645±195 | 11 | ||
| – | – | 4725±130 | – | ||
| N. Mus 91 | 0.43260249(9) | K0-4 V | VIS SPEC | 4950±330 | 12 |
| K3-5 V | VIS SPEC | 4645±195 | 13 | ||
| K3-4 V | VIS SPEC | 4730±110 | 14 | ||
| K4-6 V | VIS SPEC | 4410±210 | 15 | ||
| – | – | 4685±70 | – | ||
| MAXI J1305-704 | 0.394(4) | – | SPEC FIT | 4610±145 | 16 |
| GS 2000+25 | 0.3440915(9) | K3-7 V | VIS SPEC | 4445±395 | 17 |
| K3-6 V | VIS SPEC | 4520±320 | 18 | ||
| – | – | 4485±158 | – | ||
| A 0620-00 | 0.32301415(7) | K5-7 V | VIS SPEC | 4250±200 | 19 |
| K4-5 V | VIS SPEC | 4535±85 | 20 | ||
| K3-7 V | VIS SPEC | 4445±395 | 21 | ||
| K3-4 V | VIS SPEC | 4730±110 | 22 | ||
| K0-5 V | NIR SPEC | 4865±415 | 23 | ||
| K3-5 Vb | SED | 4600±200 | 24 | ||
| – | SPEC FIT | 4900±100 | 25 | ||
| K5-7 V | NIR SPEC | 4250±200 | 26 | ||
| K4-6 Vc | NIR SPEC | 4410±210 | 27 | ||
| – | SPEC FIT | 5000±100 | 28 | ||
| – | – | 4598±45 | – | ||
| XTE J1650-500 | 0.3205(7) | K1-7 Vd | VIS SPEC | 4620±500 | 29 |
| N. Vel 93 | 0.285206(1) | K0-5 V | VIS SPEC | 486±415 | 30 |
| K7-M0 V | VIS SPEC | 3950±100 | 31 | ||
| – | – | 4407±142 | – | ||
| XTE J1859+226 | 0.276(3) | K5-7 V | VIS SPEC | 4250±200 | 32 |
| K5-7 V | VIS SPEC | 4250±200 | 33 | ||
| – | – | 4250±88 | – | ||
| GRO J0422+32 | 0.2121600(2) | M0-5 V | VIS SPEC | 3450±400 | 34 |
| M0-4 V | VIS SPEC | 3520±325 | 35 | ||
| M1-4 V | VIS SPEC | 3440±240 | 36 | ||
| M4-5 V | VIS SPEC | 3125±75 | 37 | ||
| M0-2 V | SED | 3700±150 | 38 | ||
| – | – | 3448±70 | – | ||
| XTE J1118+480 | 0.16993404(5) | K7-M0 V | VIS SPEC | 3950±100 | 39 |
| K5-M1 V | VIS SPEC | 4065±385 | 40 | ||
| K5-9 Ve | SED | 4165±285 | 41 | ||
| – | SPEC FIT | 4700±100 | 42 | ||
| K7-M1 V | NIR SPEC | 3865±185 | 43 | ||
| – | – | 4148±66 | – | ||
| SWIFT J1753.5-0127 | 0.1358(8) | M4-5 V | VIS SPEC | 3125±75 | 44 |
References. (1) Harlaftis & Greiner (2004); (2) Casares & Charles (1994); (3) Hynes et al. (2009); (4) Khargharia et al. (2010); (5) González Hernández et al. (2011); (6) Casares et al. (2004); (7) Heida et al. (2017); (8) Orosz et al. (2011); (9) Torres et al. (2019); (10) Remillard et al. (1996); (11) Harlaftis et al. (1997); (12) Remillard et al. (1992); (13) Orosz et al. (1996); (14) Casares et al. (1997); (15) Wu et al. (2015); (16) Mata Sánchez et al. (2021); (17) Casares et al. (1995a); (18) Harlaftis et al. (1996); (19) Oke (1977); (20) Murdin et al. (1980); (21) McClintock & Remillard (1986); (22) Marsh et al. (1994); (23) Shahbaz et al. (1999a); (24) Gelino et al. (2001); (25) González Hernández et al. (2004); (26) Froning et al. (2007); (27) Harrison et al. (2007); (28) Zheng et al. (2022); (29) Orosz et al. (2004); (30) Shahbaz et al. (1996); (31) Filippenko et al. (1999); (32) Corral-Santana et al. (2011); (33) Yanes-Rizo et al. (2022); (34) Orosz & Bailyn (1995); (35) Casares et al. (1995b); (36) Harlaftis et al. (1999); (37) Webb et al. (2000); (38) Gelino & Harrison (2003); (39) Wagner et al. (2001); (40) McClintock et al. (2001); (41) Gelino et al. (2006); (42) González Hernández et al. (2008a); (43) Khargharia et al. (2013); (44) Yanes-Rizo et al. (2025).
Notes. (a) Although (11) report K3-M0, the clear lack of TiO bands in their spectra strongly suggests ≲K5. (b)We adopt an uncertainty of ±1 sub-types on the spectral classification favoured by (24). (c) We adopt an uncertainty of ±1 sub-types on the spectral classification favoured by (26). (d) The spectral type is poorly constrained by (28) because of limited quality spectra and thus we adopt a conservative uncertainty of ±3 sub-types. (e) Following (26) we adopt an uncertainty of ±2 sub-types on the favoured spectral classification.
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