\begin{table}%t1
\caption{\label{table1}Properties of our luminous obscured quasars.}
%%\centering

\par
\begin{tabular}{l  l   c  c  c  c  c  c  c}  
\hline\hline \noalign{\smallskip}
Complete name & Abbreviation & 2--10~keV flux\tablefootmark{a}    & $R$\tablefootmark{b} & $K_{\rm s}$\tablefootmark{c}   & X/O & $z$\tablefootmark{d}& $N_{\rm H}$\tablefootmark{e}  & $L_{2-10~{\rm keV}}$\tablefootmark{f}\\\hline
 HELLAS2XMM 054022.0-283139  & PKS~0537\#43        &     3.35 &    22.70  &   17.50   &1.10   &1.797  &$\rm 10.5^{9.4}_{4.8}$&  6.8   \\
HELLAS2XMM 053920.4-283721    & PKS~0537\#11a        &     4.19  &    23.40  &   18.25   &1.48   &0.981  & $\rm 1.3^{1.5}_{0.9}$&  1.9\\
 HELLAS2XMM 053917.1-283819   &PKS~0537\#164       &     1.50  &    23.60  &   19.02   &1.12   & 1.824 & --&3.1 \\
 HELLAS2XMM 053851.3-283949    &PKS~0537\#123       &     2.97  &    23.10  &   17.94   &1.21   & 1.153 & $\rm 6.6^{21.6}_{4.1}$& 2.0\\
  HELLAS2XMM 003413.8-115559       & GD~158\#62          &     3.59  &   23.30   &   21.83&1.38   & 1.568 & $\rm 26.3^{44.7}_{18.1}$& 4.9\\
 HELLAS2XMM 003357.2-120039      &GD~158\#19          &     2.43  &   21.80   &   --      &0.63   & 1.957 & $\rm 7.3^{11.7}_{5.5}$ & 6.3 \\
 HELLAS2XMM 204428.7-105629      &Mrk~509\#01         &     2.10  &   23.85   &   17.88   &1.36   &1.049  & $<$1.1&1.5   \\
 HELLAS2XMM 204349.7-103243      &Mrk~509\#13         &     3.10  &   23.99   &   18.79   &1.59   & 1.261 & $\rm 2.5^{4.6}_{2.2}$ & 2.6\\
 HELLAS2XMM 235956.6-251019  &Abell~2690\#75      &    3.30   &   24.60   &   18.33  &1.85   & $\rm 1.3^{+0.30}_{-0.20}$\tablefootmark{\dagger}   &$\rm 15.0^{20.0}_{8.5}$&3.2 \\
HELLAS2XMM 031343.5-765426    &  PKS~0312\#36   &    1.90  &   24.70   &   19.13  &1.66   & $\rm 0.9^{+0.05}_{-0.15}$\tablefootmark{\dagger}   &$\rm 1.0^{1.2}_{0.9}$&0.7\\
HELLAS2XMM 054021.1-285037   & PKS~0537\#91   &    4.2   &   23.70   &   18.99  &1.60   & 1.538 &$\rm 45.9^{102.0}_{36.0}$&8.1\\
 HELLAS2XMM 053945.2-284910  &PKS~0537\#54   &    2.1   &   25.10   &   18.91  &1.86   &$>$1.3\tablefootmark{\dagger}    & -- &2.0\\
HELLAS2XMM 053911.4-283717   &PKS~0537\#111  &   2.1 & 24.50 & 17.64 &1.62  & $\rm 1.2^{+0.20}_{-0.10}$\tablefootmark{\dagger} &$\rm 9.1^{12.4}_{5.3}$&1.7\\
HELLAS2XMM 000111.6-251202  &Abell~2690\#29      &    2.8   &   25.10   &   17.67  &1.99   & 2.08   &$\rm 2.1^{2.6}_{1.6}$ & 8.4  \\
HELLAS2XMM 031018.9-765957   & PKS~0312\#45& 2.8 & 24.40 & 18.62  &1.70 & $\rm 1.85^{+0.20}_{-0.30}$\tablefootmark{\dagger}   & $\rm 8.0^{8.4}_{4.6}$&6.2\\
HELLAS2XMM 005030.7-520046  &BPM~16274\#69       &    2.27   &   24.08   &   17.87  &1.48   & 1.35   & $\rm 2.5^{1.5}_{1.0}$ & 2.4\\
\hline
\end{tabular}
\tablefoot{\tablefoottext{a}{Fluxes in units of $10^{-14}$~erg~cm$^{-2}$\ s$^{-1}$ from \cite{2004A&A...421..491P} 
(with the exception of BPM~16274\#69, from Lanzuisi et al., in 
preparation);}
\tablefoottext{b}{magnitude from \cite{2003A&A...409...79F} (with the 
exception of source BPM~16274\#69, from \citealt{2007A&A...466...31C});}
\tablefoottext{c}{for a sub-sample of sources, the 
$K_{\rm s}$-band analysis can be found in \cite{2004A&A...418..827M};} 
\tablefoottext{d}{spectroscopic redshift from optical spectroscopy 
(\citealt{2003A&A...409...79F}) and, for three sources, from near-IR spectroscopy (Abell~2690\#29 and BPM~16274\#69 from 
\citealt{2006A&A...445..457M}; PKS~0537\#91 from Sarria et~al., in preparation); photometric redshifts (\tablefoottext{\dagger}{symbol}), and corresponding 1$\sigma$ errors, 
from \cite{2007A&A...468..603P};}
\tablefoottext{e}{column densities in source rest-frame in units of 10$^{22}$~cm$^{-2}$ measured 
from \xray\ spectral fitting (see \citealt{2004A&A...421..491P}; and 
Lanzuisi et al., in preparation). 
For the sources with photometric redshifts, values are taken from 
\cite{2007A&A...468..603P}. For PKS~0537\#164 the \xray\ spectral 
fitting is prevented by the few \xray\ counts; for Mrk~509\#01, only an upper 
limit was derived (\citealt{2004A&A...421..491P}); for 
PKS~0537\#54, the column density is $9.3\times 10^{22}$~cm$^{-2}$ for $z= 1.3$. Galactic absorption 
column densities adopted in the spectral fitting are: 
$8\times 10^{20}$~cm$^{-2}$ for the field PKS~0312$-$77; 
$2\times 10^{20}$~cm$^{-2}$ for the field Abell~2690; $2.1\times 10^{20}$~cm$^{-2}$ for the field PKS~0537$-$28; $4\times 10^{20}$~cm$^{-2}$ for the field Mrk~509; $2.5\times 10^{20}$~cm$^{-2}$ 
for the field GD~158$-$100 (see \citealt{1992ApJS...79...77S});}
\tablefoottext{f}{rest-frame, absorption-corrected, \xray\ luminosity in units of 10$^{44}$~erg~s$^{-1}$ from \cite{2004A&A...421..491P} and from \cite{2007A&A...468..603P} for sources with photometric redshifts. 
Luminosities are computed using $H_{0}=70$~km~s$^{-1}$~Mpc$^{-1}$, $\Omega_{\rm m}=0.3$ and $\Omega_{\Lambda}=0.7$.}} \vspace*{1.5mm}
\end{table}