\begin{table} \par %%%%\centering \par \caption{Spectral fitting and X-ray fluxes at Earth for archival and {\it XMM}-{\sc epic} data of WR~25. \label{arch_fit}} \begin{tabular}{cccccrrccc} \hline\hline obs.& $N_1^{\rm H}$ & $N_2^{\rm H}$ & $kT_1$ & $kT_2$ & $\chi^2_{\rm red}$ & n.p.$^b$& \multicolumn{3}{c}{$f_{\rm x}$ ($10^{-12}$~erg~s$^{-1}$~cm$^{-2}$)} \\ \hline % & & & & & & & & & \\ \cline{2-5} \cline{8-10} % & & & & & & & & & \\[-2mm] no. & \multicolumn{2}{c}{(10$^{22}$~cm$^{-2}$)} & \multicolumn{2}{c}{(keV)} & & & [0.5--2.4~keV] & [2.4--10.0~keV] & [0.5--10.0~keV] \\ \hline & & & & & & & & & \\[-2mm] 1 & $\rm 1.03_{-0.32}^{+0.32}$ & - & $\rm 0.42_{-0.25}^{+0.25}$ & - & 13.55/19 & 0.63 & $\rm 2.13_{-0.92}^{+0.26}$ & - & - \\[+2mm] 2 & $\rm 0.91_{-0.10}^{+0.10}$ & - & $\rm 0.56_{-0.10}^{+0.10}$ & - & 17.94/19 & 0.33 & $\rm 2.14_{-0.24}^{+0.18}$ & - & - \\[+2mm] 3 & $\rm 0.96_{-0.18}^{+0.19}$ & - & $\rm 0.52_{-0.14}^{+0.17}$ & - & 17.20/19 & 0.37 & $\rm 2.67_{-0.51}^{+0.33}$ & - & - \\[+2mm] 4 & $\rm 0.95_{-0.14}^{+0.11}$ & - & $\rm 0.56_{-0.09}^{+0.14}$ & - & 17.55/19 & 0.35 & $\rm 2.36_{-0.14}^{+0.29}$ & - & - \\[+2mm] % & & & & & & & & & \\[-2mm] % & & & & & & & & & \\[-2mm] 5 & $\rm 1.05_{-0.33}^{+0.33}$ & $\rm 0.48_{-0.42}^{+0.42}$ & $\rm 0.71_{-0.22}^{+0.22}$ & $\rm 2.58_{-0.78}^{+0.78}$ & 406/647 & 1.00 & $\rm 1.73_{-0.77}^{+1.59}$ & $\rm 1.46_{-0.71}^{+0.72}$ & $\rm 3.19_{-1.48}^{+2.31}$ \\[+2mm] 6 & $0.63_{-0.12}^{+0.12}$ & $0.41^a$~~~~~ & $\rm 0.79_{-0.13}^{+0.13}$ & $\rm 2.30_{-0.44}^{+0.44}$ & 397/648 & 1.00 & $\rm 2.41_{-0.45}^{+0.42}$ & $\rm 1.52_{-0.98}^{+0.50}$ & $\rm 3.93_{-1.43}^{+0.95}$ \\[+2mm] % & & & & & & & & & \\[-2mm] % & & & & & & & & & \\[-2mm] 7 & $\rm 0.68_{-0.02}^{+0.03}$ & $\rm 0.41_{-0.04}^{+0.05}$ & $\rm 0.62_{-0.01}^{+0.02}$ & $\rm 3.13_{-0.20}^{+0.13}$ & 1065/990 & 0.04 & $\rm 2.86_{-0.03}^{+0.03}$ & $\rm 1.82_{-0.05}^{+0.05}$ & $\rm 4.68_{-0.07}^{+0.07}$ \\[+2mm] 8 & $\rm 0.68_{-0.05}^{+0.05}$ & $\rm 0.41_{-0.06}^{+0.10}$ & $\rm 0.60_{-0.04}^{+0.03}$ & $\rm 2.98_{-0.31}^{+0.41}$ & 635/607 & 0.16 & $\rm 2.79_{-0.06}^{+0.05}$ & $\rm 1.81_{-0.11}^{+0.06}$ & $\rm 4.59_{-0.14}^{+0.10}$ \\[+2mm] 9 & $\rm 0.70_{-0.02}^{+0.02}$ & $\rm 0.43_{-0.04}^{+0.04}$ & $\rm 0.62_{-0.01}^{+0.02}$ & $\rm 2.65_{-0.13}^{+0.14}$ & 1398/1325 & 0.06 & $\rm 2.42_{-0.03}^{+0.03}$ & $\rm 1.43_{-0.04}^{+0.03}$ & $\rm 3.85_{-0.06}^{+0.04}$ \\[+2mm] 10 & $\rm 0.71_{-0.02}^{+0.02}$ & $\rm 0.38_{-0.04}^{+0.08}$ & $\rm 0.62_{-0.02}^{+0.01}$ & $\rm 3.01_{-0.19}^{+0.19}$ & 1398/1242 & 0.0008 & $\rm 2.42_{-0.02}^{+0.03}$ & $\rm 1.49_{-0.04}^{+0.03}$ & $\rm 3.92_{-0.07}^{+0.04}$ \\[+2mm] 11 & $\rm 0.69_{-0.03}^{+0.02}$ & $\rm 0.39_{-0.03}^{+0.04}$ & $\rm 0.61_{-0.01}^{+0.02}$ & $\rm 2.72_{-0.12}^{+0.13}$ & 1408/1357 & 0.135 & $\rm 2.45_{-0.03}^{+0.02}$ & $\rm 1.52_{-0.04}^{+0.03}$ & $\rm 3.97_{-0.05}^{+0.04}$ \\[+2mm] 12 & $\rm 0.77_{-0.05}^{+0.06}$ & $\rm 0.24_{-0.07}^{+0.08}$ & $\rm 0.61_{-0.03}^{+0.02}$ & $\rm 2.83_{-0.48}^{+0.28}$ & 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 & $\rm 0.63_{-0.05}^{+0.05}$ & $\rm 0.32_{-0.05}^{+0.06}$ & $\rm 0.60_{-0.02}^{+0.02}$ & $\rm 2.57_{-0.26}^{+0.27}$ & 727/613 & 0.001 & $\rm 2.72_{-0.25}^{+0.25}$ & $\rm 1.81_{-0.17}^{+0.17}$ & $\rm 4.53_{-0.42}^{+0.42}$ \\ \hline \end{tabular} { \begin{description} \item $^a$ 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 {\it XMM-Newton} spectra. \item $^b$ 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 $\chi^2_{\rm red}$. \end{description} } \end{table}