Table 2
Results of the fits to the average spectra extracted by using all the available exposure time in obs1 and obs2.
| Parameter | Value | Unit |
|
|
||
| N H | 43.1  |
× 1020 cm-2 |
| A O | 0.96 ± 0.01 | Solar |
| A Fe | 0.75 ± 0.05 | Solar |
| k T in a | 0.127 ± 0.003 | keV |
a
|
66.4 |
km |
| k T nthComp b | 0.257 ± 0.010 | keV |
| Γ | 1.428 ± 0.003 | |
| N nthComp | 3.035 ± 0.005 | × 10-2 |
| E Fe | 6.6 ± 0.1 | keV |
| σ Fe | 1.08 ± 0.11 | keV |
| N Fe | 5.1 ± 0.4 | × 10-4 cm-2 s-1 |
| E O vii | 0.5719  |
keV |
| σ O vii | 0 – | keV |
| N O vii | 37 ± 11 | × 10-4 cm-2 s-1 |
| Flux1 [0.5–11 keV]c | 3.123 ± 0.007 | × 10-10 erg cm-2 s-1 |
| Flux2 [0.5–11 keV]c | 3.033 ± 0.010 | × 10-10 erg cm-2 s-1 |
 /d.o.f. |
1.1297/4067 | |
|
|
||
| E 1 d | 1.67  |
keV |
| N 1 d | 2.8 ± 1.0 | × 10-5 cm-2 s-1 |
| E 2 d | 1.85 ± 0.03 | keV |
| N 2 d | 5 ± 2 | × 10-5 cm-2 s-1 |
| E 3 d | 2.250 ± 0.010 | keV |
| N 3 d | 11.3 ± 1.6 | × 10-5 cm-2 s-1 |
Notes. The model used for the fits comprises a photoelectric absorption with variable abundances of iron and oxygen (tbnew_feo, Wilms et al. 2001), a thermal Comptonization (compTH in xspec), a thermal disk black-body, a narrow Gaussian line representing the blend pf O vii emission lines, and a broad Gaussian iron line for the iron emission. The spectra of the two observations were fit together to achieve the most stringent constraints on the X-ray emission properties. The spectra are coupled with cross-calibration constants, whose values are between 0.971 ± 0.004 and 1.09 ± 0.01.
The flux is computed from the EPIC-pn spectra and the uncertainties are only statistical, the absolute flux calibration of an X-ray camera has typical uncertainty of a few percent (e.g., Romano et al. 2005).
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