Table 1.
Log of the quiescent observations used in our paper and results of the spectral fitting.
| Observatory | Obs ID | Date | MJD | Exposure | Count |  |
FX(c) | LX(c) | |
|---|---|---|---|---|---|---|---|---|---|
| time (a) | rate (b) | (eV) | (×10−14 | (×1032 | |||||
| (ks) | (×10−3 counts s−1) | erg cm−2 s−1) | erg s−1) | ||||||
| After Outburst I | |||||||||
| 1 | Chandra | 2688 | 2001 Oct 15 | 52197.7 | 17.9 | 52.1 ± 1.7 | 111.1 ± 1.3 | 35.4 ± 1.9 | 34.3 ± 1.8 |
| 2 | Chandra | 3794 | 2002 Oct 26 | 52563.0 | 26.2 | 9.6 ± 0.6 | 79.5 ± 1.6 | 7.5 ± 0.8 | 7.3 ± 0.8 |
| 3 | XMM-Newton | 0153190101 | 2003 Mar 13 | 52711.6 | 8.2, 31.1, 13.1 | 11.3 ± 1.4, 2.6 ± 0.3, 2.4 ± 0.5 | 73.0 ± 1.9 | 5.0 ± 0.7 | 4.8 ± 0.6 |
| 4 | Chandra | 3795 | 2003 May 9 | 52768.7 | 25.6 | 3.7 ± 0.4 | 67.8 ± 2.1 | 3.4 ± 0.6 | 3.3 ± 0.6 |
| 5 | Chandra | 5469/6337 (d) | 2005 Jul 15 | 53566.4 | 45.5 | 1.0 ± 0.2 | 55.5 ± 2.4 | 1.2 ± 0.3 | 1.2 ± 0.3 |
| 6 | Chandra | 8984 | 2008 Apr 27 | 54583.8 | 26.6 | 0.9 ± 0.2 | 54.8 ± 3.2 | 1.1 ± 0.4 | 1.1 ± 0.4 |
| After Outburst II | |||||||||
| 1 | Swift | Interval 1 (e) | 2017 Mar 10 | 57822.0 | 6.6 | 1.8 ± 0.5 | 91.5 ± 8.8 | 13.4 ± 6.3 | 13.0 ± 6.1 |
| 2 | XMM-Newton | 0803640301 | 2017 Mar 23 | 57835.8 | 5.3, 22.4, 20.5 | 32.4 ± 2.7, 6.6 ± 0.6, 6.2 ± 0.6 | 87.9 ± 1.4 | 11.4 ± 1.0 | 11.1 ± 0.9 |
| 3 | Chandra | 19599 | 2017 Apr 25 | 57868.0 | 26.4 | 5.7 ± 0.5 | 82.7 ± 2.0 | 8.8 ± 1.2 | 8.6 ± 1.2 |
| 4 | Chandra | 19600 | 2017 Jul 3 | 57937.6 | 25.2 | 3.1 ± 0.4 | 74.8 ± 2.5 | 5.5 ± 1.0 | 5.3 ± 1.0 |
| 5 | XMM-Newton | 0803640401 | 2017 Aug 22 | 57987.3 | 2.2, 14.3, 21.2 | 20.0 ± 0.3, 3.1 ± 0.5, 1.7 ± 0.3 | 75.1 ± 2.4 | 5.7 ± 0.9 | 5.6 ± 0.9 |
| 6 | Chandra | 19601 | 2018 Feb 2 | 58151.5 | 26.4 | 1.4 ± 0.2 | 66.0 ± 3.0 | 3.0 ± 0.8 | 2.9 ± 0.8 |
| 7 | Chandra | 19602 | 2018 Jul 15 | 58314.4 | 38.2 | 0.5 ± 0.1 | 56.3 ± 4.2 | 1.3 ± 0.6 | 1.3 ± 0.6 |
Notes. All errors are stated for the 90% confidence level. The NH is fixed to 3.4 × 1021 cm−2. For the XMM-Newton spectra, all the model parameters (except the normalisation constant) were tied between the three detectors for a given observation. The XMM-Newton exposure times and count rates are displayed as “pn, MOS1, MOS2”. We assume that the source is at a distance of 9 kpc.
The exposure times listed are the effective ones, after the data were modified for background flaring and eclipses.
The flux and luminosity correspond to the unabsorbed flux and luminosity for the 0.5–10 keV energy range.
The spectra from these two Chandra observations have been combined; see Sect. 2.2.3.
Five Swift/XRT observations have been combined as Interval 1; see Sect. 2.2.1.
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