Table 6: Spectral fitting and X-ray fluxes at Earth for archival and XMM- EPIC data of WR 25.
obs. $N_1^{\rm H}$ $N_2^{\rm H}$ kT1 kT2 $\chi^2_{\rm red}$ n.p.b $f_{\rm x}$ (10-12 erg s-1 cm-2)
no. (1022 cm-2) (keV)     [0.5-2.4 keV] [2.4-10.0 keV] [0.5-10.0 keV]
1 $\rm 1.03_{-0.32}^{+0.32}$ - $\rm0.42_{-0.25}^{+0.25}$ - 13.55/19 0.63 $\rm 2.13_{-0.92}^{+0.26}$ - -
2 $\rm0.91_{-0.10}^{+0.10}$ - $\rm0.56_{-0.10}^{+0.10}$ - 17.94/19 0.33 $\rm 2.14_{-0.24}^{+0.18}$ - -
3 $\rm0.96_{-0.18}^{+0.19}$ - $\rm0.52_{-0.14}^{+0.17}$ - 17.20/19 0.37 $\rm 2.67_{-0.51}^{+0.33}$ - -
4 $\rm0.95_{-0.14}^{+0.11}$ - $\rm0.56_{-0.09}^{+0.14}$ - 17.55/19 0.35 $\rm 2.36_{-0.14}^{+0.29}$ - -
5 $\rm 1.05_{-0.33}^{+0.33}$ $\rm0.48_{-0.42}^{+0.42}$ $\rm0.71_{-0.22}^{+0.22}$ $\rm 2.58_{-0.78}^{+0.78}$ 406/647 1.00 $\rm 1.73_{-0.77}^{+1.59}$ $\rm 1.46_{-0.71}^{+0.72}$ $\rm 3.19_{-1.48}^{+2.31}$
6 0.63-0.12+0.12 0.41a      $\rm0.79_{-0.13}^{+0.13}$ $\rm 2.30_{-0.44}^{+0.44}$ 397/648 1.00 $\rm 2.41_{-0.45}^{+0.42}$ $\rm 1.52_{-0.98}^{+0.50}$ $\rm 3.93_{-1.43}^{+0.95}$
7 $\rm0.68_{-0.02}^{+0.03}$ $\rm0.41_{-0.04}^{+0.05}$ $\rm0.62_{-0.01}^{+0.02}$ $\rm 3.13_{-0.20}^{+0.13}$ 1065/990 0.04 $\rm 2.86_{-0.03}^{+0.03}$ $\rm 1.82_{-0.05}^{+0.05}$ $\rm 4.68_{-0.07}^{+0.07}$
8 $\rm0.68_{-0.05}^{+0.05}$ $\rm0.41_{-0.06}^{+0.10}$ $\rm0.60_{-0.04}^{+0.03}$ $\rm 2.98_{-0.31}^{+0.41}$ 635/607 0.16 $\rm 2.79_{-0.06}^{+0.05}$ $\rm 1.81_{-0.11}^{+0.06}$ $\rm 4.59_{-0.14}^{+0.10}$
9 $\rm0.70_{-0.02}^{+0.02}$ $\rm0.43_{-0.04}^{+0.04}$ $\rm0.62_{-0.01}^{+0.02}$ $\rm 2.65_{-0.13}^{+0.14}$ 1398/1325 0.06 $\rm 2.42_{-0.03}^{+0.03}$ $\rm 1.43_{-0.04}^{+0.03}$ $\rm 3.85_{-0.06}^{+0.04}$
10 $\rm0.71_{-0.02}^{+0.02}$ $\rm0.38_{-0.04}^{+0.08}$ $\rm0.62_{-0.02}^{+0.01}$ $\rm 3.01_{-0.19}^{+0.19}$ 1398/1242 0.0008 $\rm 2.42_{-0.02}^{+0.03}$ $\rm 1.49_{-0.04}^{+0.03}$ $\rm 3.92_{-0.07}^{+0.04}$
11 $\rm0.69_{-0.03}^{+0.02}$ $\rm0.39_{-0.03}^{+0.04}$ $\rm0.61_{-0.01}^{+0.02}$ $\rm 2.72_{-0.12}^{+0.13}$ 1408/1357 0.135 $\rm 2.45_{-0.03}^{+0.02}$ $\rm 1.52_{-0.04}^{+0.03}$ $\rm 3.97_{-0.05}^{+0.04}$
12 $\rm0.77_{-0.05}^{+0.06}$ $\rm0.24_{-0.07}^{+0.08}$ $\rm0.61_{-0.03}^{+0.02}$ $\rm 2.83_{-0.48}^{+0.28}$ 643/619 0.244 $\rm 2.72_{-0.27}^{+0.27}$ $\rm 1.75_{-0.18}^{+0.18}$ $\rm 4.47_{-0.45}^{+0.45}$
13 $\rm0.63_{-0.05}^{+0.05}$ $\rm0.32_{-0.05}^{+0.06}$ $\rm0.60_{-0.02}^{+0.02}$ $\rm 2.57_{-0.26}^{+0.27}$ 727/613 0.001 $\rm 2.72_{-0.25}^{+0.25}$ $\rm 1.81_{-0.17}^{+0.17}$ $\rm 4.53_{-0.42}^{+0.42}$
a Signal-to-noise ratio in the hard part of the spectrum for this observation is so low that no reliable column density can be found. Thus, we fixed it at a value similar to that derived from XMM-Newton spectra.
b n.p.: null hypothesis probability, i.e., the probability that purely random deviations of the data from the model would result in obtained or higher value of $\chi^2_{\rm red}$.


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