Table A.3.
Spectral best-fit parameters of the ten time windows of the XMM-Newton observation, using tbabs×zbbody, with their 90% confidence intervals.
| Time window | kT | Norm | L0.2-2 keV | Radius |
|---|---|---|---|---|
| (eV) |
 |
t(×1042 erg s−1) | (×106 km) | |
| 0 (1-4 combined) | 70.1 |
1.81 |
3.2 |
1.04 |
| 1 | 100.8 |
0.6 |
1.1 |
0.29 |
| 2 | 63.8 |
2.3 |
4.0 |
1.42 |
| 3 | 78.4 |
1.2 |
2.2 |
0.69 |
| 4 | 56.1 |
5.0 |
8.4 |
2.71 |
| 5 | 53.5 |
11.9 |
19.7 |
4.58 |
| 6 | 68.5 |
15.1 |
26.6 |
3.16 |
| 7 | 85.9 |
26.5 |
48.3 |
2.67 |
| 8 | 106.5 |
38.7 |
71.7 |
2.09 |
| 9 | 113.1 |
58.5 |
108.6 |
2.28 |
| 10 | 113.8 |
64.1 |
118.9 |
2.35 |
Notes. The time window 0 results from the merging of the time windows 1–4 and corresponds to the quiescent state. The bolometric black-body luminosity is computed by using the normalisation. The 0.2–2 keV luminosity is then computed by using the temperature obtained from the fitted data in the 0.3–0.9 keV band. The radius is computed by replacing zbbody with zashift×bbodyrad, which allows us to retrieve the emitting area in the normalisation factor. The spectral fitting of the time windows 1–10 resulted in a fit statistic of CStat = 341.48 with 341 degrees of freedom. The combined quiescent state fit yields a fit statistic of CStat = 34.64 with 33 degrees of freedom. For slices 0, 5, and 6, the low signal prevents us from using CStat as a direct estimate of the goodness of fit. The Monte Carlo simulations of the best-fit spectra we performed confirmed the quality of the fit. We found percentages of the worst realisation of the fits of 12% for the quiescent state, and of 68% and 4% for the first two eruption slices, respectively, the latter being marginally acceptable.
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