\begin{table}%t5
\par
\caption{Best-fit parameters for the X-ray spectral analysis (extragalactic objects).}
\label{xraymodel}
%\centerline
 {\begin{tabular}{l c l r r l l r  r }
          \hline\hline
name & id & Model & $\Gamma$ & $N_{\rm H}$   & $kT$         & red $\chi^2$/d.o.f. & $f_{2{-}10~\rm keV}$ & Log $L_{2{-}10~\rm  keV}$\\ 
     &    &   &          & ($\times$10$^{22}$) &      &         &($\times$10$^{-13}$) & \\
%     &    &   &          &[cm$^{-2}$]& [keV]&         &  [erg s$^{-1}$ cm$^{-2}$] &[erg s$^{-1}$] \\
            \hline
XBS~J002618.5$+$105019 & BEL AGN & PL &  $\rm 2.02^{+ 0.07}_{-0.06}$ & $<$  0.011 & ... & 1.15 /  97 &   2.8 & 44.44 \\
XBS~J013240.1$-$133307 & NEL AGN &PL & 1.9 (frozen) &    $\rm 2.54^{+   0.71}_{  -0.56}$ & ... & 1.11 /  19 &   1.7 & 44.41 \\
XBS~J013944.0$-$674909 & BEL AGN &PL &  $\rm 1.94^{+ 0.14}_{-0.12}$ & $<$  0.018 & ... & 0.91 /  34 &   1.2 &  42.56 \\
XBS~J015957.5$+$003309 & BEL AGN &PL &  $\rm 2.14^{+ 0.09}_{-0.09}$ & $<$  0.010 & ... & 1.19 /  99 &   2.9 &  44.03 \\
XBS~J021640.7$-$044404 & BEL AGN &PL &  $\rm 2.24^{+ 0.08}_{-0.09}$ & $<$  0.020 & ... & 1.17 /  67 &   1.1 & 44.74 \\
XBS~J021808.3$-$045845 & BEL AGN &PL + BB &  $\rm 2.01^{+ 0.04}_{-0.04}$ & $<$  0.007 &   $\rm 0.16^{+  0.01}_{ -0.01}$ & 1.07 / 527 &   2.3 & 44.79 \\
XBS~J021817.4$-$045113 & BEL AGN &PL &  $\rm 1.84^{+ 0.04}_{-0.03}$ & $<$0.04 & ... & 1.07 / 346 &   2.7 &  45.22 \\
$\rm XBS~J021822.2$-$050615^a$ & NEL AGN &Leaky &  $\rm 1.66^{+ 0.34}_{-0.36}$ &   $\rm 20.54^{+   0.36}_{  -0.44}$ & ... & 1.41 /  63 &  3.0 & 42.76 \\
XBS~J023713.5$-$522734 & NLSy1 &PL + BB &  $\rm 1.90^{+ 0.18}_{-0.13}$ & $<$  0.18 &   $\rm 0.11^{+  0.02}_{ -0.02}$ & 0.86 /  80 &   2.7 & 43.52  \\
XBS~J030206.8$-$000121 & BEL AGN &PL &  $\rm 1.90^{+ 0.06}_{-0.06}$ & $<$  0.015 & ... & 1.14 / 125 &   2.2 & 44.63\\
$\rm XBS~J030614.1$-$284019^b$ & BEL AGN &PL &  $\rm 1.56^{+ 0.26}_{-0.13}$ & $<$  0.048 & ... & 1.15 /  16 &   2.9 & 43.87 \\
XBS~J031015.5$-$765131 & BEL AGN &PL &  $\rm 1.92^{+ 0.04}_{-0.04}$ & $<$  0.022 & ... & 0.90 / 189 &   3.4 & 45.47 \\
XBS~J031146.1$-$550702 & Sy1.9 &PL &  $\rm 2.08^{+ 0.13}_{-0.12}$ & $<$  0.013 & ... & 0.93 /  44 &   2.8 &  43.37 \\
XBS~J031859.2$-$441627 &BEL AGN & PL & $\rm 1.58^{+ 0.29}_{-0.29}$ & $\rm 0.33^{+0.43}_{-0.19}$ & ... & 0.73 /  18 &   1.7 &  42.99 \\
XBS~J033845.7$-$352253 & NEL AGN &Leaky + RS & 1.9 (frozen) &   $\rm 28.5^{+   6.7}_{-10.0}$ &   $\rm 0.16^{+  0.04}_{ -0.08}$ & 0.83 /  29 &   1.7 &  43.21 \\
XBS~J040658.8$-$712457 & Sy1.9 & PL & 1.9 (frozen) &   $\rm 21.97^{+  17.67}_{  -12.78}$ & ... & 1.25 /   4 &   1.6 &  43.56 \\
XBS~J040758.9$-$712833 & NEL AGN &Leaky &  1.9 (frozen) &   $\rm 28.23^{+21.96}_{-14.64}$ & ... & 1.13 /   5 &   2.5 & 43.44 \\
XBS~J041108.1$-$711341 & BEL AGN &PL &  $\rm 1.95^{+ 0.48}_{-0.36}$ & $<$  0.61 & ... & 0.99 /   6 &   0.8 & 44.59 \\
XBS~J185613.7$-$462239 & BEL AGN &PL &  $\rm 2.18^{+ 0.27}_{-0.24}$ & $<$  0.058 & ... & 1.15 /  26 &   1.4 &  44.69 \\
XBS~J193248.8$-$723355 & ELG & PL & 1.9 (frozen) &    $\rm 1.14^{+   0.25}_{  -0.21}$ & ... & 1.06 /  35 &   1.9 &  43.76 \\
XBS~J204043.4$-$004548 & NEL AGN &PL & 1.9 (frozen) &    $\rm 3.00^{+   1.15}_{  -0.90}$ & ... & 1.35 /  16 &   1.7 & 44.50 \\
XBS~J205635.7$-$044717 & BEL AGN &PL + BB &  $\rm 1.91^{+ 0.51}_{-0.35}$ & $<$  0.56 &   $\rm 0.15^{+  0.03}_{ -0.03}$ & 1.18 /  21 &   1.7 &  43.42 \\
XBS~J205829.9$-$423634 & NLSy1 &PL &  $\rm 1.91^{+ 0.09}_{-0.09}$ &    $\rm 0.09^{+   0.04}_{  -0.03}$ & ... & 0.76 / 120 &   3.2 &  43.76 \\
XBS~J213002.3$-$153414 & BEL AGN &PL &  $\rm 2.10^{+ 0.23}_{-0.21}$ &    $\rm 0.08^{+   0.12}_{  -0.08}$ & ... & 0.82 /  26 &   1.8 &  44.45 \\
$\rm XBS~J213824.0$-$423019^c$ & BEL AGN &PL &  $\rm 2.14^{+ 0.25}_{-0.17}$ & $<$  0.057 & ... & 0.86 /  26 &   1.6 & 43.60 \\
XBS~J214041.4$-$234720 & BEL AGN &PL &  $\rm 2.19^{+ 0.10}_{-0.10}$ & $<$  0.012 & ... & 1.06 /  93 &   1.7 & 44.28 \\
XBS~J220601.5$-$015346 &BEL AGN & PL + BB &  $\rm 1.56^{+ 0.16}_{-0.09}$ & $<$0.670 & $\rm 0.06^{+  0.01}_{ -0.04}$ & 0.72 /  15 &   1.7 & 43.36 \\
                        \hline
\end{tabular}}
\par
Column 1: source name;
\par
Col. 2: optical identification;
\par
Col. 3: best-fit model (PL = absorbed power-law; Leaky = leaky absorbed power-law;
PL + BB = absorbed power-law plus Black-Body spectrum; Leaky + RS = leaky absorbed power-law plus a Raymond-Smith
spectrum)
\par
Col. 4: best-fit photon index of the power-law component;
\par
Col. 5: best-fit intrinsic hydrogen column density [cm$^{-2}$];
\par
Col. 6: temperature of the thermal component (if present) [keV];
\par
Col. 7: reduced Chi-squared and degrees of freedom of the best-fit;
\par
Col. 8: observed 2--10~keV flux (corrected for the Galactic absorption) [erg~s$^{-1}$~cm$^{-1}$];
\par
Col. 9: logarithm of the intrinsic luminosity in the 2--10~keV energy range [erg~s$^{-1}$];
\par
$^a$ results from the X-ray analysis taken from Severgnini et~al. (\cite{Severgnini03});
\par
$^b$ in this object the presence of an emission line at 1.9~keV 
(source rest frame, consistent with the Si XIII at 1.86~keV) is required;
\par
$^c$ in this object the presence of an emission line at 6.4~keV 
(source rest frame, consistent with the Fe I K$\alpha$) 
is required. 
\end{table}