Table B.2.
Parameter constraints from fitting the data within each epoch with a power–law model.
| Model | Parameter | Epoch 1 | Epoch 2 | Epoch 3 | Epoch 4 | Epoch 5 | Epoch 6 |
| Constant | CFPMA | [1.0] | |||||
| CFPMB | - | 1.01 ± 0.03 | 0.92 ± 0.04 | 1.00 ± 0.06 | - | - | |
| CSwift | - | 0.95 ± 0.07 | 0.47 ± 0.08 | 0.9 ± 0.1 | - | - | |
| CXMM − Newton | - | - | - | 0.78 ± 0.04 | - | - | |
| TBabs | NH (1020 cm−2) | [5.0] | |||||
| powerlaw | Γ | - | 1.38 ± 0.02 | 1.52 ± 0.05 | 1.68 ± 0.01 | 1.7 ± 0.2 | 2.4 ± 0.7 |
| norm (keV−1cm−2s−1) | - | (10.0 ± 0.5)×10−4 | (4.2 ± 0.4)×10−4 | (3.9 ± 0.2)×10−4 | (3.7 ± 0.4)×10−6 | (1.2 ± 0.4)×10−6 | |
| C-stat/d.o.f. | - | 256.8/267 | 174.0/158 | 221.0/231 | 47.0/33 | 12.0/9 | |
Notes. We use a constant model to account for differences in normalization between each instrument and fix the constant for NuSTAR/PFMA spectra CFPMA = 1 in each epoch. The total fit function is thus "constant*TBabs*powerlaw". Parameter values held fixed during the fit are given inside square brackets. No parameter constraints are given for Epoch 1, because at this epoch the source X–rays are dominated by reflection. With time the source spectrum seems to become softer.
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