\begin{table}%t4
\caption{\label{t4}Synoptic table containing the main results concerning the 11
AGNs (Figs. 5--7) identified or observed in the present sample of 
{\it INTEGRAL} sources.}
%\centerline
{
\begin{tabular}{lcccccrcr}
\hline
\hline
\multicolumn{1}{c}{Object} & $F_{\rm H_\alpha}$ & $F_{\rm H_\beta}$ &
$F_{\rm [OIII]}$ & Class & $z$ &
\multicolumn{1}{c}{$D_L$ (Mpc)} & $E(B-V)_{\rm Gal}$ & \multicolumn{1}{c}{$L_{\rm X}$} \\
\hline
IGR J00333+6122 & * & 2.5 $\pm$ 0.6 & 1.76 $\pm$ 0.09 & Sy1.5 & 0.105 & 522.2 & 1.231 & 22 (2--10) \\
 & * & [90 $\pm$ 20] & [58 $\pm$ 3] & & & & & 39 (20--100) \\
 %& & & & & & & & \\
Swift J0216.3+5128 & --- & --- & 0.24 $\pm$ 0.03 & likely Sy2 & 0.422 & 2492.1 & 0.187 & 890 (0.2--12) \\
 & --- & --- & [0.36 $\pm$ 0.05] & & & & & 970 (2--10) \\
 & & & & & & & & 1100 (20--100) \\
 %& & & & & & & & \\
IGR J02466$-$4222 & in abs. & in abs. & $<$5.0 & XBONG & 0.0695 & 337.4 & 0.018 & $\sim$0.1 (0.5--8) \\
 & [in abs.] & [in abs.] & [$<$5.6] & & & & & 42 (17--60) \\
% & & & & & & & & \\
IGR J02524$-$0829 & 2.6 $\pm$ 0.3 & in abs. & 2.4 $\pm$ 0.2 & Sy2 & 0.0168 & 78.5 & 0.054 & 0.35 (2--10) \\
 & [2.8 $\pm$ 0.3] & [in abs.] & [2.7 $\pm$ 0.3] & & & & & 2.3 (17--60) \\
% & & & & & & & & \\
IGR J05270$-$6631 & --- & --- & --- & Type 1 & 0.978 & 6922.4 & 0.075 & 280 (0.1--2) \\
 & --- & --- & --- & QSO & & & & 11 (2--10) \\
 & & & & & & & & 5600 (20--40) \\
 & & & & & & & & $<$6300 (40--100) \\
 %& & & & & & & & \\
IGR J09025$-$6814 & in abs. & in abs. & $<$2.6 & XBONG & 0.014 & 63.4 & 0.101 & 0.0072 (2--10) \\
 & [in abs.] & [in abs.] & [$<$3.8] & & & & & 1.2 (20--100) \\
 & & & & & & & & \\
IGR J09253+6929 & * & 23 $\pm$ 5 & 13.2 $\pm$ 0.7 & Sy1.5 & 0.039 & 185.2 & 0.290 & 0.25 (2--10) \\
 & * & [55 $\pm$ 11] & [31.6 $\pm$ 1.6] & & & & & 4.3 (20--40) \\
 & & & & & & & & $<$4.3 (40--100) \\
% & & & & & & & & \\
IGR J10147$-$6354 & * & 37 $\pm$ 2 & 9.8 $\pm$ 0.5 & Sy1.2 & 0.202 & 1067.2 & 0.314 & 29 (2--10) \\
 & * & [81 $\pm$ 4] & [21.8 $\pm$ 1.1] & & & & & $<$31 (20--40) \\
 & & & & & & & & 160 (40--100) \\
 %& & & & & & & & \\
IGR J12415$-$5750 & * & 42 $\pm$ 7 & 88 $\pm$ 3 & Sy1.5 & 0.024 & 113.7 & 0.609 & 0.52 (0.1--2.4) \\
 & * & [300 $\pm$ 70] & [588 $\pm$ 18] & & & & & 2.3 (0.2--12) \\
 & & & & & & & & 3.5 (20--100) \\
 %& & & & & & & & \\
IGR J16426+6536 & --- & 1.89 $\pm$ 0.09 & 0.78 $\pm$ 0.04 & NLSy1 & 0.323 & 1821.3 & 0.021 & 44 (0.2--12) \\
 & --- & [2.0 $\pm$ 0.1] & [0.81 $\pm$ 0.04] & & & & & 910 (20--40) \\
 & & & & & & & & $<$790 (40--100) \\
 %& & & & & & & & \\
IGR J18249$-$3243 & * & $<$0.9 & 9.6 $\pm$ 0.9 & Sy1 & 0.355 & 2033.2 & 0.233 & 38 (0.1--2.4) \\
 & * & [$<$1.5] & [14.5 $\pm$ 1.5] & & & & & 260 (2--10) \\
 & & & & & & & & 390 (20--100) \\
\hline
\end{tabular}}
\par
\medskip
Note: emission line fluxes are reported both as  observed and (between square brackets) corrected for the intervening Galactic absorption $E(B-V)_{\rm Gal}$ along the object line of sight  
(from Schlegel et~al. 1998). Line fluxes are in units of 10$^{-15}$ erg cm$^{-2}$ s$^{-1}$, whereas X-ray luminosities are in units of 10$^{43}$ erg s$^{-1}$ and the reference band (between round brackets) is expressed in keV. The typical error on the redshift measurement is $\pm$0.001 but for the SDSS and 6dFGS spectra, for which an uncertainty of $\pm$0.0003 can be assumed.\\
$^*$ Heavily blended with [N {\sc ii}] lines.
\end{table}