Table 3.
Results.
| # | Source | Mmin | Lexp, GR | Lexp, GR + MB |  |
d | Method | dm, GR | dm, GR + MB |
|---|---|---|---|---|---|---|---|---|---|
| M⊙ | (1035 erg s−1) | (1035 erg s−1) | (1033 erg s−1) | (kpc) | (kpc) | (kpc) | |||
| S1 | IGR J18245–2452 | 0.21 | 0.21 | 1.40 | 1.32(13) | 5.5 [4] | GC | 3.97(19) | 10.2(5) |
| S2 | Swift J1749.4–2807 | 0.60 | 1.70 | 12.0 | 0.23(2) | < 8 [13] | B | 27.1(1.4) | 71.0(4.0) |
| S3 | IGR J17591–2342 | 0.43 | 2.20 | 13.0 | 5.2(5) | < 7 [14] | M | 6.7(0.3) | 16.1(0.8) |
| S4 | SAX J1748.9–2021 | 0.12 | 0.11 | 0.44 | 45.0(4.) | 8.5 [8] | GC | 0.50(2) | 0.99(5) |
| S5 | XTE J1814–338 | 0.20 | 3.20 | 5.40 | 0.49(5) | < 9.6 [10] | B | 25.7(1.3) | 33.2(1.7) |
| S6 | IGR J17498–2921 | 0.20 | 1.80 | 3.70 | 0.61(6) | 7.6 [7] | B | 17.4(0.8) | 24.8(1.2) |
| S7 | IGR J17511–3057 | 0.16 | 2.50 | 3.80 | 2.30(20) | < 7 [1] | B | 10.4(5) | 12.8(6) |
| S8 | IGR J00291+5934 | 0.04 | 0.35 | 0.41 | 0.98(9) | < 4.7 [2] | B | 6.0(3) | 6.4(3) |
| S9 | SAX J1808.4–3658 | 0.008 | 0.95 | 1.01 | 14.0(1.4) | 3.5 [3] | B | 2.63(13) | 2.77(14) |
| S10 | IGR J1737.9–3747 | 0.07 | 2.30 | 2.50 | 2.20(20) | < 4 [14] | M | 10.1(4) | 10.6(4) |
| S11 | HETE J1900.1–2455 | 0.018 | 0.32 | 0.33 | 790.0(80) | < 5 [5] | B | 0.20(1) | 0.20(1) |
| S12 | NGC 6440 X–2 | 0.0005 | 0.17 | 0.18 | 0.144(14) | 8.5 [8] | GC | 11.0(4) | 11.0(4) |
| S13 | Swift J1756.9–2508 | 0.008 | 0.19 | 0.20 | 0.41(4) | < 14 [14] | M | 6.9(7) | 7.0(7) |
| S14 | IGR J16597–3704 | 0.007 | 0.25 | 0.25 | 2.5(2) | 9.1 [11] | GC | 3.14(16) | 3.15(16) |
| S15 | MAXI J0911–655 | 0.027 | 4.00 | 4.05 | 8.9(9) | 9.5 [12] | GC | 6.7(7) | 6.7(7) |
| S16 | XTE J0929–314 | 0.01 | 0.55 | 0.56 | 0.80(8) | U | – | 8.3(6) | 8.4(6) |
| S17 | XTE J1751–305 | 0.016 | 1.50 | 1.50 | 1.16(12) | < 8.5 [9] | T | 11.4(4) | 11.5(4) |
| S18 | XTE J1807–294 | 0.0077 | 0.41 | 0.42 | 5.7(6) | U | – | 2.70(13) | 2.71(13) |
| S19 | IGR J17062–6143 | 0.0060 | 0.29 | 0.29 | 10.0(1.0) | 7.3 [6] | B | 1.66(8) | 1.66(8) |
Notes. List of the obtained expected and observed luminosities for the selected sample of AMXPs. The minimum masses for the companion star Mmin reported in this table have been inferred from the mass function of the source fixing i to 60°, with the exception of the eclipsing Swift J1749.4−2807, for which i was fixed to 90°. In the table, Lexp, GR and Lexp, GR + MB are the expected luminosity evaluated for a mass transfer driven by GR and GR+MB, respectively, Fav is the bolometric (0.1–300 keV) unabsorbed flux averaged over 20 years, d the distance known for the system, and dm, GR and dm, GR + MB the distances evaluated using Lexp, GR and Lexp, GR + MB respectively. The label “U” indicates that the distance of the source is unknown at the moment. The cited values for d are upper limits on the distance, therefore we reported the value found on the refereed paper plus its upper error. In the “Method” column we indicate the method used to determine the upper limit on d reported here.
Methods: “B”: study of type-I X-ray bursts. “GC”: association to a globular cluster of known distance. “M”: study of the extinction maps by Marshall et al. (2006). “T”: theoretical argument.
References. [1] = Altamirano et al. (2010b), [2] = De Falco et al. (2017a), [3] = Galloway & Cumming (2006), [4] = Harris et al. (1996), [5] = Kawai & Suzuki (2005), [6] = Keek et al. (2017), [7] = Linares et al. (2011), [8] = Ortolani et al. (1994), [9] = Papitto et al. (2008), [10] = Strohmayer et al. (2003), [11] = Valenti et al. (2007), [12] = Watkins et al. (2015), [13] = Wijnands et al. (2009), [14] = This paper.
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