Table 2.
Best-fit results from Model 5: TBabs*(expabs*powerlaw+diskbb+rfxconv*nthComp).
| NB | FB | |
|---|---|---|
| Component | ||
| TBABS | ||
| nH (1022) | 0.3 (frozen) | 0.3 (frozen) |
| POWERLAW | ||
| PhoIndex | 2 (frozen) | 2 (frozen) |
| norm |
 |
0.5 ± 0.3 |
| RFXCONV | ||
| rel_refl | 0.20 ± 0.03 | 0.14 ± 0.02 |
| log ξ |
 |
 |
| DISKBB | ||
| Tin (keV) | 0.55 ± 0.03 | 0.64 ± 0.03 |
| Rdisc (km) | 122 ± 27 | 89 ± 15 |
| NTHCOMP | ||
| Gamma | 2.49 ± 0.03 |
 |
| kTe (keV) |
 |
 |
| kTbb (keV) | 0.92 ± 0.02 |
 |
| norm |
 |
 |
| τ | 7.2 ± 0.2 | 6.0 ± 0.3 |
| Rseed (km) | 39 ± 4 | 26 ± 3 |
| χ2/d.o.f. | 1316/1183 | 1149/1101 |
Notes. The parameters Fe_abun (iron abundance), z (redshift), and CosIncl (cosine of the inclination angle) of RFXCONV were kept fixed to the values of 1, 0, and 0.6947, respectively. The uncertainties were calculated at 90% c.l. The spectral parameters are defined as in XSPEC. To estimate the value of the inner radius of the accretion disc Rdisc, we made the same assumptions as reported for Model 3B. The optical depth τ of the electron corona was estimated using the relation provided by Zdziarski et al. (1996), and for the seed-photon emitting radius Rseed, we applied the form by in ’t Zand et al. (1999).
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