Table B.2.
Parameter constraints derived from fitting the spectrum at each epoch with one or two black bodies.
| Model | Parameter | X2–p | X2–v | X3–p | X3–v |
|---|---|---|---|---|---|
| constant | CMOS | 0.94 ± 0.07 | 0.8 ± 0.1 | 0.97 ± 0.08 | 1.1 ± 0.1 |
| TBabs | NH (1020 cm−2) | [2.6] | [2.6] | [2.6] | [2.6] |
| zbbody1 | kTe (keV) | 0.14 ± 0.01 | 0.14 ± 0.01 | 0.11 ± 0.01 | 0.13 ± 0.01 |
| Normzbb1 (1037(1 + z)−2 erg/s/kpc2) | (3.6 ± 0.3)×10−6 | (1.7 ± 0.1)×10−6 | (2.7 ± 0.3)×10−6 | (1.4 ± 0.1)×10−6 | |
| zbbody2 | kTe (keV) | 0.3 ± 0.2 | - | 0.20 ± 0.04 | - |
| Normzbb2 (1037(1 + z)−2 erg/s/kpc2) |
 |
- |
 |
- | |
| C-stat/d.o.f. | 52.0/43 | 14.3/17 | 35.3/42 | 25.1/18 | |
Notes. Same as Table B.1, but here we fit the time–resolved spectra at the peaks (X2–p and X3–p) and the valleys (X2–v and X3–v). See Fig. 5 for the production of those spectra. Due to the decrease of the source flux below the background level, we only consider the energy range of 0.3–1.0 keV for the X2–v and X3–v spectra in the analysis. It is not possible to detect the second, hotter black body in X2–v and X3–v. We find the best–fit temperature of the primary black body to be consistent with being the same in the peak and valley spectra.
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