Table 3.
Spectral analysis results for the power-law model fitting.
| ObsID | Regime | Γ | FX | LX |
|---|---|---|---|---|
| (10−13 erg cm−2 s−1) | (1033 erg s−1) | |||
| 2007 | ||||
| 0505280101 | Out of periastron | 2.73 ± 0.19 | 1.28 |
0.792 |
| 2015/2016 | ||||
| 000311720[30]a | Out of periastron | 0.435 ± 0.089 | 938 |
582 |
| +[31]a | " | 1.52 ± 0.25 | 45.6 |
28.3 |
| +[32–33] | " | 1.75 ± 0.28 | 19.7 |
12.2 |
| +[34–35] | Periastron | 2.40 ± 0.39 | 16.8 |
10.4 |
| +[36] | " | 0.232 ± 0.067 | 746 |
463 |
| +[37–40] | Out of periastron | 1.84 |
9.5 |
5.88 |
| +[41] | Periastron | 2.36 |
11.0 |
6.8 |
| +[42–43] | Out of periastron | 2.3 ± 1.2 | 5.8 |
3.57 |
| +[44] | Periastron | 2.62 |
8.9 |
5.5 |
| 0790180301 | Out of periastron | 2.369 ± 0.082 | 2.43 ± 0.14 | 1.506 |
| 000311720[46] | Periastron | 1.49 ± 0.33 | 5.35 |
3.32 |
| 2017/2018 | ||||
| 000311720[63]a | Out of periastron | 0.496 ± 0.093 | 585 |
363 |
| +[64–65] | " | 2.09 |
11.9 |
7.4 |
| +[66] | Periastron | 4.02 |
64.0 |
40 |
| +[67] | " | 1.87 |
41.6 |
25.8 |
| +[74] | Out of periastron | 1.50 |
8.7 |
5.39 |
| +[75] | " | 2.34* | 2.06 |
1.28 |
| +[77-78] | " | 2.08 |
4.0 |
2.46 |
| +[79] | Periastron | 0.68 |
31.7 |
19.7 |
| +[80–81] | Out of periastron | 3.05 |
6.49 |
4.03 |
| 0804940201 | " | 2.34 |
1.28 |
0.93 |
| +[83] | Periastron | 0.70 |
28.1 |
17.4 |
| +[84] | " | 1.20 |
5.1 |
3.2 |
| +[85–87] | Out of periastron | 3.83 |
6.1 |
3.8 |
Notes. The NH was fixed to 9 × 1021 cm−2 (Kalberla et al. 2005). The FX and LX are calculated in the 0.5–10 keV energy range and using a distance of ∼7.2 kpc (Rouco Escorial et al. 2018). All errors are expressed for 1σ confidence interval. The * indicates that the parameters was fixed to the given value during the spectral fits. The observations indicated with the awere obtained during the decay phase of the giant outbursts and not during the low-luminosity states. The results for these observations are listed for comparison.
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