Table 2.
Best-fit parameters of the EPIC-pn spectra during flares and quiescence in the 2016 XMM-Newton observations.
| Model parameters(a) | obs1F(b) | obs1Q(b) | obs2F(b) | obs2Q(b) | obs3F(b) | obs3Q(b) |
|---|---|---|---|---|---|---|
| Γ | 1.9 |
1.9(c) | 1.9(c) | 1.9(c) | 1.9(c) | 1.9(c) |
| PL flux(d) (10−14erg cm−2 s−1) | 3.7 ± 0.4 | 1.5 ± 0.3 | 3.3 ± 0.7 | 1.4 ± 0.2 | 3.3 ± 0.9 | 1.1 ± 0.2 |
| kTin (eV) | 143 ± 7 | 143(c) | 143(c) | 143(c) | 143(c) | 143(c) |
| Rin (e) (km) | 6400 |
< 1100 | 6300 |
< 1100 | 4200 ± 600 | < 900 |
| O VIII norm.(f) (10−6 photons cm−2 s−1) | 4.2 ± 1.0 | 0.6 ± 0.4 | 4.3 ± 1.2 | 0.5 ± 0.3 | 5.7 ± 1.3 | 0.4 ± 0.3 |
Notes. (a)The model is TBabs*(pegpwrlw + diskbb + gaussian) with absorption fixed to NH=1.55 × 1020 cm−2 and the emission line centroid and width fixed to 0.65 keV and 0, respectively. All uncertainties are at 1 σ and 
for 267 d.o.f. (b)F and Q indicate flaring and quiescent time intervals, respectively, during observations 0761630101 (obs1), 0761630201 (obs2), and 0761630301 (obs3). (c)Linked parameter. (d)Unabsorbed flux of the power-law component in the 0.3–10 keV energy band. (e)Apparent inner radius of the diskbb model, assuming a disk inclination of 45°. (f)Flux of Gaussian emission line with E = 0.65 keV and σ = 0.
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