\begin{table}%t3
\caption{\label{xspec}Results from X-ray data analysis and spectral fitting.}
\par
%\centering
\par
\begin{tabular}{lrrcccrrlll}
\hline \hline \noalign{\smallskip}
SDSS Name& Cts& HR& $N_{\rm H}^{\rm gal}$& $N_{\rm H}$& $\Gamma$& $\chi^2/{\rm d.o.f.}$& $f_{2-10}$& $L^{\rm abs}_{2-10}$& $L^{\rm int}_{2-10}$& Class\\
(1)& (2)& (3)& (4)& (5)& (6)& (7)& (8)& (9)& (10)& (11)\\ 
\hline \noalign{\smallskip}
J105951.36+301817.4&  237& --0.30& 2.0& $\rm 1.84^{+1.05}_{-0.75}$& $\rm 1.90^{+0.40}_{-0.35}$& 25.6/20&    16&    44.70&    44.80&      thin\\
J092640.67+023628.7&   65& --0.06& 3.8& $\rm 4.40^{+4.00}_{-2.70}$& $\rm 1.67^{+0.75}_{-0.65}$&     ...&   6.8&    44.61&    44.75&      thin?\\
J034222.54--055727.9&  175& --0.50& 5.3& $\rm 0.70^{+0.77}_{-0.57}$& $\rm 1.83^{+0.56}_{-0.45}$& 10.4/13&    13&    44.60&    44.61&      thin\\
J104603.17+071907.2&   31& --0.16& 2.8& $\rm 3.10^{+2.22}_{-1.59}$&          $1.8^{\rm fixed}$&     ...&   3.7&    44.04&    44.15&     thin?\\
J165158.61+432508.6&  313& --0.38& 1.9& $\rm 0.72^{+0.55}_{-0.44}$& $\rm 1.76^{+0.33}_{-0.30}$& 20.7/27&    19&    44.76&    44.79~&      thin\\
J080859.33+204711.8&   18&  0.80& 4.0&                    ...&   $\rm --1.2^{+0.9}_{-1.4}$&     ...&   14&    43.95&    45.65$^*$& thick\\
J125848.58+120531.1&   18& --0.05& 2.2&    $\rm 2.5^{+3.0}_{-1.8}$&          $1.8^{\rm fixed}$&     ...&   1.8&    43.88&    43.97&     thin?\\
J145503.94+515539.9&  125& --0.43& 1.8& $\rm 0.36^{+0.98}_{-0.36}$& $\rm 1.82^{+0.58}_{-0.41}$&  14.4/9&   5.7&    44.67&    44.69&      thin\\
J085600.88+371345.5& ${<}4$& .....& 2.9&                    ...&                    ...&     ...&$<$2.0& $<$43.50& $<$45.20$^*$& thick\\
\hline		
\end{tabular}
\tablefoot {Column description: (1) Source name. (2) Net counts in the 0.5$-$8~keV band. (3) Hardness ratio, defined as (H$-$S)/(H+S), where H and S are the number of photons observed in the 0.5$-$2~keV and 2$-$8~keV bands, respectively. (4) Galactic column density in units of $10^{20}$~cm$^{-2}$ \citep{dl90}. (5) Absorbing column density at the source redshift in units of $10^{22}$~cm$^{-2}$. (6) Photon index. (7) Chi-square value over number of degrees of freedom: for sources with less than 100~net counts C-statistics has been used. (8) Observed 2$-$10~keV flux in units of $10^{-14}$~erg~cm$^{-2}$~s$^{-1}$. (9) Logarithm of the 2$-$10~keV rest frame luminosity, not corrected for absorption, in units of erg~s$^{-1}$. (10)~Logarithm of the intrinsic 2$-$10~keV rest frame luminosity, i.e.~corrected for absorption, in~units of erg~s$^{-1}$; $^*$ for the two candidate Compton-thick objects it is assumed $L^{\rm int} = 50$~$\times$ $L^{\rm obs}$ (see~text). (11) Object classification based on the X-ray spectral analysis and the X/NeV~ratio.}
\vspace*{6mm}
\end{table}