\begin{table}%t3
\par
\caption{\label{tab3}X-ray spectral properties of the 23 sources showing a detection in at least one of the two energy bands, S and H.}
%\centerline
{
\begin{tabular}{cccccccccc}
\hline\hline 
\multicolumn{1}{c} {ID}&
\multicolumn{1}{c} {CR$_{0.5-2}$}&
\multicolumn{1}{c} {CR$_{2-10}$}&
\multicolumn{1}{c} {HR}&
\multicolumn{1}{c} {Flux$_{2-10}$}&
\multicolumn{1}{c} {$N_{\rm H}$}&
\multicolumn{1}{c} {log($L_{\rm X,obs}$)}&
\multicolumn{1}{c} {log($L_{\rm X}$)}&            
\multicolumn{1}{c} {log($\lambda L_{5.8}$/\lum)}&
\multicolumn{1}{c} {Analysis} \\
(1)  &  (2) & (3) & (4) & (5) & (6) & (7) & (8) & (9) & (10) 
 \\\hline 
1  &  $19.4 \pm3.4$  &  $6.1 \pm2.5$   & --$0.52\pm0.19$ & $\rm 10.2_{-4.0}^{+3.8}$    & $\rm 1.1_{-0.7}^{+1.4}$       &  43.68  &  43.72         &      1.4 1  & SP\\
4  &  $1.7  \pm0.8$  &  $2.2 \pm0.9$   &  $0.13\pm0.31$   & $\rm 8.5_{-4.2}^{+5.9}$     & $\rm 19.9_{-14.4}^{+37.8}$    &  43.90  &  44.31         &      1.31   & SP\\ 
5  &  $2.7  \pm1.3$  &  $1.8 \pm1.2$   & --$0.25\pm0.53$ & $\rm 2.2_{-0.6}^{+2.8}$     & $<$14.3                   &  42.93  &  43.03         &      2.1    & SP\\ 
6  &  $21.1 \pm2.5$  &  $63.7\pm4.3$   &  $0.49\pm0.07$   & $\rm 113.1_{-30.0}^{+17.0}$ & $\rm 10.8_{-3.8}^{+3.6}$      &  44.49  &  44.71         &      0.95   & SP\\ 
7  &  $4.0  \pm2.8$  &  $7.4 \pm3.9$   &  $0.30\pm0.44$   & $\rm 14.2_{-3.0}^{+3.0}$    & $\rm 25.0_{-23.0}^{+35.0}$    &  44.40  &  44.48         &      1.43   & HR\\ 
8  &  $<$6.9         &  $4.8  \pm4.1$  &  $>$--0.53        & $\rm 3.4_{-1.6}^{+1.6}$     & $>$0.1                    &  43.13  &  $>$43.13$^a$  &      1.29   & HR\\ 
9  &  $1.8  \pm1.6$  &  $2.8 \pm1.9$   &  $0.21\pm0.54$   & $\rm 5.3_{-1.9}^{+1.9}$     & $\rm 25.0_{-24.0}^{+60.0}$    &  44.08  &  44.15         &      1.47   & HR\\ 
10 &  $1.0  \pm0.9$  &  $<$1.5         &  $<$0.25         & $<$$\rm 2.3_{-1.4}^{+1.4}$  & $<$6.0                    &  42.82  &  42.87         &      1.76   & HR\\ 
11 &  $5.0  \pm2.3$  &  $3.5 \pm2.4$   & --$0.18\pm0.39$ & $\rm 5.8_{-2.7}^{+2.6}$     & $\rm 4.9_{-4.0}^{+9.9}$       &  43.40  &  43.57         &      1.73   & SP\\ 
12 &  $1.9  \pm1.6$  &  $5.7 \pm2.5$   &  $0.50\pm0.44$   & $\rm 27.1_{-3.9}^{+4.8}$    & $\rm 267.9_{-144.8}^{+274.7}$ &  43.40  &  45.16         &      0.34   & SP\\ 
19 &  $2.2  \pm1.3$  &  $8.6 \pm4.4$   &  $0.60\pm0.62$   & $\rm 12.6_{-7.9}^{+7.9}$    & $\rm 25.0_{-17.0}^{+75.0}$    &  44.10  &  44.92         &      1.76   & HR\\ 
21 &  $13.0 \pm5.3$  &  $10.6 \pm4.9$  & --$0.10\pm0.31$ & $\rm 24.8_{-6.4}^{+6.4}$    & $\rm 4.0_{-3.5}^{+8.0}$       &  44.19  &  44.21         &      1.05   & HR\\ 
22 &  $5.9  \pm3.0$  &  $6.7 \pm3.7$   &  $0.06\pm0.37$   & $\rm 11.3_{-4.2}^{+4.2}$    & $\rm 13.0_{-11.0}^{+35.0}$    &  44.35  &  44.39         &      1.56   & HR\\ 
25 &  $10.9 \pm3.7$  &  $4.5  \pm5.0$  & --$0.42\pm0.43$ & $\rm 18.6_{-3.8}^{+3.8}$    & $<$45.0                   &  45.26  &  45.30         &      1.33   & HR\\ 
31 &  $<$2.2         &  $0.9  \pm0.4$  &  $>$--0.15        & $\rm 1.7_{-0.7}^{+0.7}$     & $>$0.1                    &  43.24  &  $>$43.24$^a$  &      1.70   & HR\\ 
32 &  $0.7  \pm0.3$  &  $1.8 \pm0.5$   &  $0.49\pm0.31$   & $\rm 3.1_{-0.5}^{+0.5}$     & $\rm 75.0_{-40.0}^{+75.0}$    &  44.10  &  44.53         &      2.23   & HR\\ 
33 &  $0.7  \pm0.3$  &  $1.9 \pm0.6$   &  $0.48\pm0.28$   & $\rm 3.8_{-0.6}^{+0.6}$     & $\rm 60.0_{-30.0}^{+45.0}$    &  44.10  &  44.59         &      1.82   & HR\\ 
36 &  $3.7  \pm2.5$  &  $9.4 \pm3.8$   &   $0.43\pm0.40$  & $\rm 4.3_{-1.2}^{+6.6}$     & $<$28.0                   &  43.01  &  43.06         &      1.21   & SP\\ 
39 &  $11.2 \pm2.8$  &  $25.9 \pm3.9$  &  $0.40\pm0.14$   & $\rm 29.9_{-13.4}^{+7.4}$   & $\rm 6.7_{-2.4}^{+3.5}$       &  43.65  &  43.85         &      1.03   & SP\\ 
40 &  $23.2 \pm3.5$  &  $6.9  \pm2.3$  & --$0.53\pm0.16$ & $\rm 9.3_{-1.3}^{+2.1}$     & $<$1.5                    &  43.88  &  43.90         &      1.34   & SP\\ 
41 &  $4.6  \pm1.9$  &  $17.5\pm2.8$   &  $0.58\pm0.18$   & $\rm 23.7_{-8.1}^{+6.9}$    & $\rm 11.9_{-5.0}^{+8.7}$      &  43.88  &  44.05         &      0.46   & SP\\ 
43 &  $40.7 \pm5.8$  &  $3.3  \pm3.0$  & --$0.81\pm0.18$ & $\rm 12.0_{-2.7}^{+6.6}$    & $<$0.3                    &  44.44  &  44.45         &      1.04   & SP\\ 
44 &  $31.2 \pm4.1$  &   $18.4\pm3.6$  & --$0.26\pm0.11$ & $\rm 19.5_{-7.5}^{+6.9}$    & $\rm 1.7_{-0.8}^{+1.1}$      & 43.94 & 44.01        &     1.24  &SP\\ 
\hline                                    
\end{tabular}}  
\par
\smallskip          
Column: 
(1) ID number; 
(2) count rate in the S band in units of $10^{-4}$ count/s;
(3) count rate in the H band in units of $10^{-4}$ count/s;
(4) Hardness Ratio between the H band and the S band computed with the formula H--S/${\rm H+S}$; 
(5) H band flux in units of $10^{-15}$ erg s$^{-1}$ cm$^{-2}$;
(6) rest-frame column density \nh~in units of $10^{22}$ cm$^{-2}$;
(7) logarithm of the observed luminosity in the H band (erg s$^{-1}$);                                 
(8) logarithm of the absorption-corrected luminosity in the H band (erg s$^{-1}$);
(9) logarithm of the $\lambda$\lcihu\/\lum~ratio;
(10) analysis method: SP for spectral fitting, HR for hardness ratio. For \chandra~data the 2$-$10~keV count rate and flux was  extrapolated from the 2$-$8~keV value assuming $\Gamma=1.9$. \\
$^a$ For these sources we computed the absorption-corrected luminosity using the lower limit on the \nh~value. Accordingly, the intrinsic luminosity shown here is also a lower limit. 
\vspace*{3mm}
\end{table}