Table 4
List of X-ray transients with 2–10 keV peak luminosities LX ≳ 1034 erg s-1 that are located in the region covered by this campaign.
| Source name | Offset from |
|
|
Comments | Rec? | Ref. |
| Sgr A∗ (′) | (erg s-1) | (erg s-1) | ||||
|
|
||||||
| CXOGC J174540.0–290031 | 0.05 | 1 × 1035 | ≲2 × 1031 | LMXB black hole candidate, radio source | No | 1, 2, 3 |
| Porb = 7.9 h, high inclination | ||||||
| CXOGC J174541.0–290014* | 0.31 | 1 × 1034 | ≲8 × 1031 | unclassified | Yes | 2 |
| CXOGC J174540.0–290005 | 0.37 | 2 × 1035 | ≲4 × 1031 | unclassified | Yes | 2, 4 |
| CXOGC J174538.0–290022 | 0.44 | 2 × 1035 | ~1 × 1033 | unclassified | Yes | 2, 5 |
| 1A 1742–289 | 0.92 | 7 × 1038 | ~5 × 1031 | LMXB black hole candidate, radio source | No | 6, 7, 19 |
| CXOGC J174535.5–290124* | 1.35 | 3 × 1034 | ≲9 × 1030 | unclassified | Yes | 2, 4, 5 |
| Swift J174535.5–285921 | 1.36 | 8 × 1034 | ~3 × 1031 | unclassified (CXOGC J174535.6–285928) | No | 19, 20, 21, 22 |
| AX J1745.6–2901* | 1.37 | 6 × 1036 | ~5 × 1032 | neutron star LMXB (burster), Porb = 8.4 h | Yes | 4, 5, 8 |
| Swift J174553.7–290347 | 4.50 | 2 × 1035 | ~7 × 1031 | unclassified (CXOGC J174553.8–290346) | No | 4 |
| XMMU J174554.4–285456 | 6.38 | 8 × 1034 | ≲2 × 1031 | unclassified, possible 172-s X-ray pulsar | No | 2, 23 |
| GRS 1741–2853* | 10.00 | 1 × 1037 | ~1 × 1032 | neutron star LMXB (burster), D = 7.2 kpc | Yes | 4, 5, 9, 10 |
| Swift J174622.1–290634 | 11.04 | 7 × 1034 | ≲7 × 1031 | unclassified (CXOGC J174622.2–290634) | No | 4 |
| XMM J174544–2913.0 | 12.56 | 5 × 1034 | ≲1 × 1032 | unclassified | No | 11 |
| XMM J174457–2850.3* | 13.78 | 2 × 1036 | ~1 × 1032 | unclassified, possible 5-s X-ray pulsar | Yes | 4, 5, 11 |
| SAX J1747.0–2853* | 19.55 | 4 × 1037 | ~2 × 1031 | neutron star LMXB (burster), D = 6.7 kpc | Yes | 12, 13 |
| GRO J1744–28* | 21.71 | 3 × 1038 | ~2 × 1033 | neutron star LMXB (0.5-s X-ray pulsar) | Yes | 14, 15, 16 |
| Porb = 11.8 d | ||||||
| KS 1741–293* | 22.09 | 5 × 1036 | ~5 × 1032 | neutron star LMXB (burster) | Yes | 17, 18 |
Notes. Table updated from Wijnands et al. (2006a). Sources marked by an asterisk were detected in an active state during our campaign. and represent the peak and quiescent luminosities, respectively. These values were taken from the literature and converted into the 2–10 keV energy band, or determined in this work. A distance of 8 kpc was assumed, except for GRS 1741–2853 and SAX J1747.0–2853, which have estimated distances of 7.2 and 6.7 kpc, respectively. The column labelled “Rec?” indicates whether a source recurred (i.e., displayed more than one distinct outburst) between 1999 and 2012.
References. 1 = Muno et al. (2005a), 2 = Muno et al. (2005b), 3 = Porquet et al. (2005a), 4 = Degenaar & Wijnands (2009), 5 = Degenaar & Wijnands (2010), 6 = Davies et al. (1976), 7 = Branduardi et al. (1976), 8 = Maeda et al. (1996), 9 = Muno et al. (2003a), 10 = Trap et al. (2009), 11 = Sakano et al. (2005), 12 = Werner et al. (2004), 13 = Wijnands et al. (2002), 14 = Giles et al. (1996), 15 = Wijnands & Wang (2002), 16 = Daigne et al. (2002), 17 = in ’t Zand et al. (1991), 18 = de Cesare et al. (2007), 19 = Muno et al. (2009), 20 = Degenaar et al. (2011b), 21 = Degenaar et al. (2011c), 22 = Chakrabarty et al. (2011), 23 = Porquet et al. (2005b).
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