Table 1.
Best fitting parameters for the burst spectra in the five intervals shown in Fig. 4.
| Parameter | 2–12 s | 12–32 s | 32–62 s | 62–112 s | 112–162 s |
|---|---|---|---|---|---|
| Model 1: Γ = 1.49, Ecut = 57.6 keV, Kpl = 0.175 | |||||
| Tbb |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
| χ2/d.o.f. | 193.6/114 | 370.1/253 | 344.9/323 | 414.5/413 | 354.6/318 |
| Model 1b: Γ = 1.49, Ecut = 57.6 keV, Kpl = 0.175, RNS = 10.88 km, log g = 14.3 | |||||
| L/LEdd |
 |
 |
 |
 |
 |
| KBURSTATMO |
 |
 |
 |
 |
 |
| χ2/d.o.f. | 128.6/114 | 290.8/253 | 319.4/323 | 425.2/413 | 354.8/318 |
| Model 2: Γ = 1.49, Ecut = 57.6 keV | |||||
| Tbb |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
| Kpl |
 |
 |
 |
 |
 |
| χ2/d.o.f. | 170.2/113 | 332.8/252 | 340.6/322 | 414.5/412 | 354.3/317 |
| Model 3: Γ = 1.49 | |||||
| Tbb |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
 |
| Kpl |
 |
 |
 |
 |
 |
| Ecut |
 |
 |
 |
 |
 |
| Fper |
 |
 |
 |
 |
 |
| χ2/d.o.f. | 105.5/112 | 279.4/251 | 306.9/321 | 405.6/411 | 353.1/316 |
| Model 3b: Γ = 1.49, RNS = 10.88 km, log g = 14.3 | |||||
| L/LEdd |
 |
 |
 |
 |
 |
| Kburstatmo |
 |
 |
 |
 |
 |
| Kpl |
 |
 |
 |
 |
 |
| Ecut |
 |
 |
 |
 |
 |
| Fper |
 |
 |
 |
 |
 |
| χ2/d.o.f. | 107.0/112 | 277.6/251 | 307.0/321 | 415.4/411 | 352.3/316 |
Notes. The Galactic absorption column was fixed to the best fitting value of the persistent emission (NH = 3.36 × 1021 cm−2). Model 1 follows the “standard” burst fitting approach, where the persistent emission parameters are not allowed to vary during the spectral fits. In Model 2 the persistent emission shape is fixed, but its normalization is allowed to vary (i.e. the Worpel et al. 2013, 2015 method). In Model 3 the cutoff energy and normalization are allowed to vary. In Model 3 and 3b the persistent flux Fper (unabsorbed in the 0.01–1000 keV range) is not a fitting parameter, but is instead calculated using the CFLUX command. For the non-burst spectrum it is 3.80 ± 0.02 × 10−9 erg cm−2 s−1, and for the burst intervals it is reported in the table.
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