Table A.1
Results of the spectral fits.
| Models tbabsism ∗ phabs ∗ (apec + gauss), or tbabsism ∗ vphabs ∗ ( ∑ vapec + gauss) for * and **, tbabsism ∗ (vphabs1 ∗ vapec1 + vphabs2 ∗ (vapec2 + gauss)) for † | |||||||
| N H | kT | norm | cente r line | strengt h line | χ2 (d.o.f.) |
|
|
| (1022 cm-2) | (keV) | (10-3 cm-5) | (keV) | (10-6 ph cm-2 s-1) | (10-11 erg cm-2 s-1) | ||
|
|
|||||||
| EPIC, C | 0.215 ± 0.002 | 11.7 ± 0.2 | 6.32 ± 0.02 | 6.371 ± 0.019 | 5.35 ± 0.86 | 1.23 (804) | 1.053 ± 0.004 |
| EPIC, A | 0.223 ± 0.003 | 10.4 ± 0.2 | 6.41 ± 0.02 | 6.355 ± 0.020 | 5.76 ± 1.24 | 1.20 (754) | 1.061 ± 0.005 |
| EPIC+RGS, A | 0.225 ± 0.003 | 10.5 ± 0.2 | 6.39 ± 0.02 | 6.355 ± 0.022 | 5.84 ± 1.18 | 1.20 (1218) | 1.057 ± 0.005 |
| EPIC+RGS, A* | 0.235 ± 0.004 | 10.5 ± 0.3 | 6.48 ± 0.02 | 6.374 ± 0.022 | 6.19 ± 1.19 | 1.15 (1217) | 1.042 ± 0.006 |
| EPIC+RGS, A** | 0.238 ± 0.004 | 1.41 ± 0.18 | 0.19 ± 0.07 | 6.372 ± 0.021 | 5.87 ± 1.19 | 1.12 (1215) | 1.050 ± 0.007 |
| 12.0 ± 0.5 | 6.36 ± 0.05 | ||||||
| EPIC+RGS, A† | 0. ± 0.03 | 1.44 ± 0.13 | 0.17 ± 0.06 | 1.11 (1214) | 1.048 ± 0.006 | ||
| 0.263 ± 0.010 | 11.6 ± 0.5 | 6.40 ± 0.04 | 6.370 ± 0.015 | 5.89 ± 1.18 | |||
| Model tbabsism ∗ phabs ∗ (pow + gauss) | |||||||
| N H | Γ | norm | cente r line | strengt h line | χ2 (d.o.f.) |
|
|
| (1022 cm-2) | (10-3 cm-5) | (keV) | (10-5 ph cm-2 s-1) | (10-11 erg cm-2 s-1) | |||
|
|
|||||||
| EPIC, C | 0.287 ± 0.004 | 1.591 ± 0.007 | 1.717 ± 0.014 | 6.680 ± 0.005 | 1.25 ± 0.10 | 1.32 (804) | 1.054 ± 0.004 |
| EPIC, A | 0.302 ± 0.003 | 1.618 ± 0.006 | 1.806 ± 0.011 | 6.685 ± 0.023 | 1.20 ± 0.14 | 1.29 (754) | 1.064 ± 0.006 |
| EPIC+RGS, A | 0.300 ± 0.004 | 1.608 ± 0.007 | 1.778 ± 0.014 | 6.676 ± 0.009 | 1.19 ± 0.14 | 1.28 (1218) | 1.062 ± 0.006 |
Notes. “EPIC” indicates a simultaneous fit of all EPIC spectra, “EPIC+RGS” a simultaneous fit of all XMM-Newton spectra; and “C” and “A” indicate EPIC extractions in a circle or annulus (see Sect. 2). The interstellar column was fixed to 3.16 × 1020 cm-2 (Gudennavar et al. 2012) and the Gaussian width to zero since these lines are not resolved by EPIC cameras. Solar abundances of Asplund et al. (2009) were used except for cases marked by (∗), (∗∗), or (†): in these cases, vapec and vphabs were used and the best-fit abundances of iron in number, relative to hydrogen and relative to the solar value amount to 
, 
, and 
respectively. Fluxes, expressed in the 0.5–10.0 keV band correspond to observed ones. Errors (found using the “error” command for the spectral parameters and the “flux err” command for the fluxes) correspond to 1σ; whenever errors were asymmetric, the highest value is provided here.
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