Table 2.
Key properties of SXTs with estimated average accretion rates and quiescent thermal luminosities.
| No. | Short name | ⟨Ṁobs⟩ |
 |
Porb | Spin | Md | Distance |
|---|---|---|---|---|---|---|---|
| (M⊙ yr−1) | (1033 erg s−1) | (h) | (Hz) | (M⊙) | (kpc) | ||
| 1 | 4U 2129+47 | 3.9 × 10−9 [1] |
 [2,3] (a) |
5.96 [1] | – | – | 10.3 ± 0.4 [4] |
| 2 | KS 1731−260 | < 9 × 10−10 [5] (b) | 0.39 ± 0.03 [6] | > 2 [7] | 524 [8] | – | 7.2 ± 1.0 [9] |
| 3 | 4U 1608−522 | 9.6 × 10−10 [11] |
 [10,11] (a) |
10 –125 [7] | 620 [8] | – | 4.1 ± 0.4 [9] |
| 4 | Ter 5 X-1 | 3 × 10−11 [12] | < 0.1 [12,13] | – | 333 [14] | – | 5.5 ± 0.9 [15] |
| 5 | 1M 1716−315 | < 2.5 × 10−10 [2] |
 [2,16] (a) |
– | – | – | 5.1 − 6.9 [17] |
| 6 | XTE J1709 | 1.8 × 10−10 [10] |
 [18] (b) |
– | – | – | 8.5 − 8.8 [18,19] |
| 7 | MXB 1659−29 | 1.4 × 10−10 [10] |
 [10,20] (a) |
7.11 [9] | 567 [8] | 0.3–0.8 [21] | 12 ± 3 [9] |
| 8 | XB 1732−304 | < 1.5 × 10−10 [10] | < 1.1 [10] | – | – | – | 5.2 ± 0.5 [22] |
| 9 | Cen X-4 | 3.8 × 10−11 [1] | 0.12 ± 0.01 [23] (b) | 15.1 [24] | – | 0.31 ± 0.27 [25] (c) | 1.2 ± 0.2 [1] |
| 10 | 1H 1905+00 | < 1.1 × 10−10 [2] | < 0.01 [2] | < 1.5 [2] | – | – | 10 [26] (d) |
| 11 | 2S 1803−245 | < 7 × 10−11 [2] | < 0.52 [2] | ∼9 [2] | – | – | 7.3 [2,27] (d) |
| 12 | 4U 1730−22 | < 4.8 × 10−11 [2] |
 [2,28] (a) |
– | – | – |
 [28] |
| 13 | EXO 1747 | < 3 × 10−11 [10] | < 0.07 [10] | – | – | – | 11 [9,29] (d) |
| 14 | XTE 2123 | < 7 × 10−12 [1] | < 0.14 [10] | 5.956 [7] | – | 0.76 ± 0.22 [30] (e) | 9.6 ± 1.3 [30] |
| 15 | SAX J1810.8 | 5 × 10−12 [31] | < 0.2 [10] | – | 532 [32] | – | 4.9 ± 0.3 [33] |
| 16 | Aql X-1 | 3.2 × 10−10 [34] (b) | 2.1 ± 0.5 [34] (b) | 18.9 [7] | 550 [7] | – | 3.0 − 6.1 [7] |
| 17 | NGC 6440 X-1 | 6 × 10−11 [35] | 1.3 ± 0.4 [36] (b) | 8.765 [37] | 442 [37] | 0.12–1 [37] | 8.5 ± 0.6 [37] |
| 18 | NGC 6440 X-2 | 8.4 × 10−13 [35] | < 0.023 [38] (b) | 0.960 [39] | 206 [39] | ∼0.0076 [39] | 8.5 ± 0.4 [40] |
| 19 | XTE J0929 | ≲2 × 10−11 [2] | < 0.1 [2] (f) | 0.726 [41] | 185 [41] | ∼0.01 [41] |
 [40] |
| 20 | SAX J1808.4 | 1.7 × 10−11 [1] | < 0.02 [2] (f) | 2.014 [42] | 401 [42] |
 [43] |
3.4 − 3.6 [1] |
| 21 | XTE J1807 | ≲3 × 10−11 [35] (g) | < 0.13 [2] | 0.667 [44] | 190.6 [44] | – | 4.4 ± 0.6 [44] |
| 22 | XTE J1751 | 4.3 × 10−12 [35] | < 0.4 [2] | 0.707 [45] | 245 [8] | 0.014–0.035 [45] |
 [40] |
| 23 | XTE J1814 | 6 × 10−12 [1] | < 0.17 [2] | 4.275 [7] | 314 [7] | 0.19–0.32 [46] (h) | 8.0 ± 1.6 [7] |
| 24 | IGR J00291 | ∼2.2 × 10−12 [47] (c) |
 [2] |
2.46 [48] | 599 [48] | 0.039–0.16 [48] | 2.6 − 3.6 [1] |
| 25 | HETE J1900.1 | 3.9 × 10−11 [35] | 0.061 ± 0.037 [49] | 1.388 [50] | 377 [50] | 0.016–0.07 [50] | 4.7 ± 0.6 [7] |
| 26 | XTE J1701 | < 9 × 10−10 [51] (b) | < 5 [51,52] (f) | – | – | – | 7.3 − 8.8 [53] |
| 27 | Ter 5 X-2 | < 1.7 × 10−11 [54] (f) | 0.7 ± 0.1 [54] | 21.274 [55] | 11.04 [55] | ≳0.4 [55] | 5.5 ± 0.9 [15] |
| 28 | EXO 0748 | < 4.4 × 10−10 [1] | 3.8 ± 0.2 [56] | 3.824 [57] | 552 [8] | ∼0.1 [58] | 7.4 ± 0.9 [9] |
| 29 | 1RXS J180408 | < 4.6 × 10−11 [59] |
 [59] (b) |
– | – | – | 5.8 [59] (d) |
| 30 | Ter 5 X-3 | < 3 × 10−11 [60] (f) | 1.2 ± 0.2 [61] (i) | – | – | – | 5.5 ± 0.9 [15] |
| 31 | SAX J1750.8 | 2 × 10−10 [62] | < 2.8 [63] | – | 601 [8] | – | 6.79 ± 0.14 [9] |
| 32 | Swift J1756.9 | 1.5 × 10−11 [35] | < 1.0 [38] (b) | 0.912 [64] | 182 [64] | 0.007–0.03 [64] | 8 ± 4 [9] |
| 33 | GRS 1747 | 1.0 × 10−10 [65] | < 2.4 [65] | 12.360 [66] | – | – |
 [4] |
| 34 | IGR J18245 | ≲10−10 [35] | < 0.07 [67] | 11.026 [68] | 254 [68] | ∼0.2 [68] |
 [68,69] |
| 35 | MAXI J0556 | < 10−9 [70] (f) | < 5.1 [71] (f) | [72] (j) | – | 0.45 [72] |
 [71] |
Notes. Each row gives the sequential number; source name (may be truncated; see Table 1 for the full identifiers); estimate of the long-term averaged mass accretion rate; observed thermal luminosity in quiescence; orbital period; estimate of the companion (donor star) mass (some mass ratio estimates are given in the footnotes); distance estimate.
References. [1] Coriat et al. (2012); [2] Heinke et al. (2009); [3] Nowak et al. (2002); [4] Kuulkers et al. (2003); [5] Ootes et al. (2016); [6] Merritt et al. (2016); [7] Watts et al. (2008); [8] Watts (2012); [9] Galloway et al. (2008); [10] Heinke et al. (2007); [11] Rutledge et al. (1999); [12] Degenaar & Wijnands (2012); [13] Rivera Sandoval et al. (2018); [14] Matrange et al. (2017); [15] Ortolani et al. (2007); [16] Jonker et al. (2007a); [17] Jonker & Nelemans (2004); [18] Degenaar et al. (2013); [19] Jonker et al. (2004); [20] Cackett et al. (2013); [21] Ponti et al. (2018); [22] Ortolani et al. (1999); [23] Cackett et al. (2010); [24] Cowley et al. (1988); [25] D’Avanzo et al. (2005); [26] Jonker et al. (2007b); [27] Cornelisse et al. (2007); [28] Tomsick et al. (2007); [29] Tomsick et al. (2005); [30] Casares et al. (2002); [31] Fiocchi et al. (2009); [32] Bilous et al. (2018); [33] Allen et al. (2018); [34] Ootes et al. (2018); [35] Van et al. (2019), accretion rate is rescaled to the canonical neutron star; [36] Walsh et al. (2015); [37] Sanna et al. (2016); [38] Haskell et al. (2012); [39] Bult et al. (2015); [40] Heinke et al. (2013); [41] Galloway et al. (2002); [42] Chakrabarty & Morgan (1998); [43] Wang et al. (2013); [44] Riggio et al. (2008); [45] Markwardt et al. (2002); [46] Wang et al. (2017); [47] De Falco et al. (2017); [48] Galloway et al. (2005); [49] Degenaar et al. (2017); [50] Kaaret et al. (2006); [51] Turlione et al. (2015); [52] Fridriksson et al. (2011); [53] Lin et al. (2009) [54] Ootes et al. (2019); [55] Papitto et al. (2011); [56] Degenaar et al. (2014) [57] Parmar et al. (1986); [58] Mikles & Hynes (2012); [59] Parikh et al. (2018); [60] Bahramian et al. (2014); [61] Degenaar et al. (2015); [62] Lowell et al. (2012); [63] Parikh & Wijnands (2017); [64] Krimm et al. (2009); [65] Vats et al. (2018); [66] in ’t Zand et al. (2003); [67] Linares et al. (2014); [68] Papitto et al. (2013); [69] Becker et al. (2003); [70] Homan et al. (2014); [71] Parikh et al. (2017); [72] Cornelisse et al. (2012).
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