\begin{table}%ta2
\caption{\label{tab:srcdata}Fit results with single powerl law model. Columns: (1) Source name; 
(2) absorbing column density  [$10^{20}$~cm$^{-2}$]; 
(3) photon index of the power law; 
(4)~normalization of the power law model [$10^{-2}$~ph~cm$^{-2}$~s$^{-1}$~keV$^{-1}$ at $1$~keV]; 
(5)~reduced $\chi^2$ and degrees of freedom;
(6) observed flux in the $0.4{-}10$~keV energy band [$10^{-11}$~erg~cm$^{-2}$~s$^{-1}$];
(7) intrinsic luminosity in the $0.4{-}10$~keV energy band rest frame [$10^{45}$~erg~s$^{-1}$].
The uncertainties in the parameter estimates are at the $90\%$ confidence limits for 1 parameter. 
For $N_{{\rm H}}={\rm Gal}$, it means that the absorption column has been fixed to the Galactic value.}
\small%\centerline
{
\begin{tabular}{lcccccc}
\hline\hline
Name         & $N_{{\rm H}}$  & $\Gamma$         & $A$              & $\tilde{\chi}^2$/d.o.f.   & $F$      & $L$\\
(1)         & (2)                & (3)               & (4)              & (5)              & (6)              & (7) \\
\hline
$0219+428$ & Gal.              & $2.60\pm 0.04$   & $0.183\pm 0.007$ & $1.29/293$     & $0.21$  & $2.6$\\
AO~$0235+164$ & Gal.              & $2.28\pm 0.02$   & $1.22\pm 0.04$   & $0.99/618$     & $0.96$  & $66$\\
PKS~$0521-365$ & Gal.              & $1.847\pm 0.009$ & $0.231\pm 0.002$ & $1.15/1202$    & $1.2$   & $9.0\times 10^{-4}$\\
S5~$0716+714^{a}$ & Gal.      & $2.58\pm 0.02$   & $0.294\pm 0.003$ & $1.74/419$     & $1.0$   & $>$$14.2$\\
S5~$0836+710^{b}$ & $14\pm 3$ & $1.379\pm 0.007$ & $2.62\pm 0.04$   & $1.07/2272$    & $4.8$   & $902$\\
Mkn~$421^{c}$ & $2.3\pm 0.3$ & $2.61\pm 0.01$ & $7.74\pm 0.09$  & $0.97/1026$    & $26.0$  & $0.59$\\
{}           & $3.5\pm 0.2$      & $2.438\pm 0.006$ & $26.3\pm 0.1$    & $1.20/1491$    & $90.6$  & $2.12$\\
{}           & $3.1\pm 0.2$      & $2.457\pm 0.006$ & $25.6\pm 0.1$    & $1.29/1430$    & $88.8$  & $2.05$\\
{}           & $3.1\pm 0.2$      & $2.373\pm 0.007$ & $18.3\pm 0.1$    & $1.12/1447$    & $66.1$  & $1.51$\\
{}           & $4.6\pm 0.2$      & $2.73\pm 0.01$   & $13.5\pm 0.1$    & $1.16/1178$    & $40.6$  & $1.02$\\
{}           & $3.7\pm 0.2$      & $2.43\pm 0.01$   & $16.3\pm 0.1$    & $1.03/1307$    & $56.0$  & $1.31$\\
PKS~$1127-145^{d}$ & $\rm 12_{-1}^{+2}$ & $1.31\pm 0.02$   & $0.34\pm 0.01$   & $1.01/890$     & $1.1$   & $59.2$\\
ON~$231$     & $2.5\pm 0.6$      & $2.77\pm 0.04$   & $0.186\pm 0.005$ & $1.07/653$     & $0.50$  & $0.16$\\
3C~$273$     & Gal.              & $1.829\pm 0.004$ & $2.788\pm 0.007$ & $1.82/1598$    & $12.2$  & $8.4$\\
{}           & Gal.              & $1.819\pm 0.005$ & $2.68\pm 0.01$   & $1.71/1401$    & $11.8$  & $8.2$\\
{}           & Gal.              & $1.812\pm 0.005$ & $2.603\pm 0.009$ & $1.53/1394$    & $11.5$  & $8.0$\\
{}           & Gal.              & $1.8\pm 0.2$     & $2.599\pm 0.004$ & $2.08/1647$    & $11.5$  & $8.0$\\
{}           & Gal.              & $1.9\pm 0.2$     & $3.634\pm 0.004$ & $4.22/1711$    & $14.5$  & $10.2$\\
{}           & Gal.              & $1.87\pm 0.01$   & $4.18\pm 0.03$   & $1.24/802$     & $17.4$  & $12.2$\\
{}           & Gal.              & $1.82\pm 0.01$   & $3.97\pm 0.03$   & $1.15/806$     & $17.5$  & $12.1$\\
{}           & Gal.              & $1.89\pm 0.01$   & $3.09\pm 0.02$   & $1.08/680$     & $12.7$  & $8.90$\\
{}           & Gal.              & $1.98\pm 0.01$   & $4.67\pm 0.03$   & $1.21/790$     & $17.7$  & $12.6$\\
{}           & Gal.              & $2.019\pm 0.009$ & $3.92\pm 0.02$   & $1.37/899$     & $14.3$  & $10.3$\\
{}           & Gal.              & $2.02\pm 0.01$   & $3.99\pm 0.03$   & $1.23/711$     & $14.5$  & $10.4$\\
{}           & Gal.              & $1.950\pm 0.009$ & $4.78\pm 0.03$   & $1.27/826$     & $18.5$  & $13.2$\\
{}           & Gal.              & $1.963\pm 0.008$ & $4.13\pm 0.02$   & $1.12/908$     & $15.8$  & $11.2$\\
{}           & Gal.              & $1.901\pm 0.009$ & $3.07\pm 0.02$   & $1.33/877$     & $12.5$  & $8.77$\\
{}           & Gal.              & $1.899\pm 0.006$ & $2.64\pm 0.01$   & $1.32/1160$    & $10.7$  & $7.54$\\
Cen~A$^{e}$ & $1400\pm 200$ & $2.2\pm 0.1$ & $\rm 22_{-5}^{+7}$   & $0.97/668$     & $16.9$  & $3.0\times 10^{-4}$\\
{}           & $1800\pm 300$         & $2.3\pm 0.2$ & $\rm 29_{-9}^{+14}$  & $0.97/340$     & $18.5$  & $3.3\times 10^{-4}$\\
PKS~$1334-127$ & $6.7\pm 0.9$      & $1.80\pm 0.04$   & $0.171\pm 0.009$ & $0.93/609$     & $0.43$  & $5.1$\\
PKS~$1406-076$ & Gal.              & $1.58\pm 0.07$   & $\rm 0.060_{-0.006}^{+0.007}$& $0.79/90$  & $0.10$ & $10.5$\\
{}           & Gal.              & $1.6\pm 0.1$     & $\rm 0.056_{-0.007}^{0.009}$ & $0.94/49$  & $0.094$ & $9.78$\\
NGC~$6251$ & $\rm 11.6_{-0.7}^{+0.8}$  & $1.94\pm 0.03$   & $0.134\pm 0.004$ & $1.04/812$     & $0.577$ & $9.6\times 10^{-3}$\\
PKS~$1830-211^{d}$ & $350\pm 50$ & $\rm 1.17_{-0.05}^{+0.03}$ & $\rm 0.62_{-0.08}^{+0.07}$ & $0.90/600$ & $1.42$ & $322$\\
{}           & $240\pm 10$         & $1.14\pm 0.02$   & $0.54\pm 0.03$   & $1.04/1662$    & $1.34$  & $290$\\
{}           & $220\pm 10$         & $1.13\pm 0.03$	  & $0.47\pm 0.03$   & $1.04/1168$    & $1.22$  & $261$\\
PKS~$2155-304^{c}$ & $1.6\pm 0.2$ & $2.592\pm 0.009$ & $5.12\pm 0.04$ & $1.02/1266$   & $14.4$  & $5.71$\\
{}           & $2.2\pm 0.2$      & $2.81\pm 0.01$   & $4.49\pm 0.04$   & $1.00/1067$    & $11.6$  & $4.87$\\
{}           & $1.9\pm 0.3$      & $2.86\pm 0.01$   & $3.61\pm 0.04$   & $1.03/991$     & $9.32$  & $3.90$\\
{}           & $3.2\pm 0.2$      & $2.868\pm 0.009$ & $8.23\pm 0.06$   & $1.01/1131$    & $20.2$  & $8.89$\\
{}           & $1.4\pm 0.3$      & $2.70\pm 0.01$   & $3.68\pm 0.05$   & $0.99/886$     & $10.0$  & $4.02$\\
{}           & $3.0\pm 0.3$      & $2.89\pm 0.01$   & $2.81\pm 0.04$   & $0.87/880$     & $6.90$  & $3.03$\\
{}           & Gal.              & $2.96\pm 0.01$   & $2.40\pm 0.01$   & $0.95/614$     & $6.17$  & $2.60$\\
{}           & $2.5\pm 0.5$      & $3.08\pm 0.02$   & $2.80\pm 0.05$   & $0.88/625$     & $6.83$  & $3.04$\\
{}           & $2.9\pm 0.4$      & $2.98\pm 0.02$   & $3.77\pm 0.05$   & $1.10/831$     & $9.14$  & $4.07$\\
\hline
\end{tabular}}
\smallskip
$^{{a}}$ Only MOS1+MOS2, since the PN was set in TIMING. Lower limit of luminosity calculated for $z=0.5$.\\
$^{{b}}$ Additional absorber placed at the redshift of the source (\texttt{wa*zwa(zpo)} model in \texttt{xspec}).\\
$^{{c}}$ Fit in the $0.6{-}10$~keV energy range and extrapolation to $0.4$~keV for flux and luminosity calculations.\\
$^{{d}}$ Additional redshifted absorber (\texttt{wa*zwa(zpo)} model in \texttt{xspec}) along the line of sight.\\
$^{{e}}$ Fit in the $4{-}10$~keV energy range, without $6{-}8$~keV energy band, because of complex features 
in the low energy part and in the iron emission line complex.
\end{table}