\begin{table}%t4
\caption{\label{tab4}Synoptic table containing the main results concerning the 18~broad emission-line AGNs (Figs.~\ref{fig8}$-$\ref{fig10}) identified or observed in the present sample of {\it INTEGRAL} sources.}
%\centering
\par
 {  {
\begin{tabular}{lcccccrcr}
\hline
\hline
\noalign{\smallskip}
\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 J00158+5605 & \tablefootmark{*} & 27.7 $\pm$ 1.3 & 30.0 $\pm$ 0.9 & Sy1.5 & 0.169 & 875.5 & 0.427 & 1.8 (0.1--2.4) \\
 & \tablefootmark{*} & [88 $\pm$ 4] & [94 $\pm$ 3] & & & & & 6.1 (0.2--2) \\
 & & & & & & & & 35 (20--40) \\
 & & & & & & & & $<$26 (40--100) \\
IGR J02086$-$1742 & \tablefootmark{*} & 120 $\pm$ 12 & 38.5 $\pm$ 1.9 & Sy1.2 & 0.129 & 651.8 & 0.028 & 1.1 (0.1--2.4) \\
 & \tablefootmark{*} & [126 $\pm$ 13] & [42 $\pm$ 2] & & & & & 33 (2--10) \\
 & & & & & & & & 140 (20--100) \\
IGR J06058$-$2755 & \tablefootmark{*} & 58 $\pm$ 6 & 66 $\pm$ 3 & Sy1.5 & 0.090 & 443.1 & 0.030 & 5.0 (0.1--2.4) \\
 & \tablefootmark{*} & [64 $\pm$ 6] & [72 $\pm$ 4] & & & & & 30 (0.2--12) \\
 & & & & & & & & 36 (17--60) \\
Swift J0845.0$-$3531 & \tablefootmark{*} & 26.3 $\pm$ 1.3 & 5.4 $\pm$ 0.3 & Sy1.2 & 0.137 & 695.7 & 0.531 & 5.9 (0.1--2.4) \\
 & \tablefootmark{*} & [112 $\pm$ 6] & [22.9 $\pm$ 1.6] & & & & & 78 (14--150) \\
 & & & & & & & & 50 (17--60) \\
IGR J09094+2735 & \tablefootmark{*} & 4.7 $\pm$ 0.3 & 1.36 $\pm$ 0.04 & NLSy1 & 0.2844 & 1572.4 & 0.030 & 6.7 (0.1--2.4) \\
 & \tablefootmark{*} & [4.8 $\pm$ 0.3] & [1.51 $\pm$ 0.05] & & & & & 920 (17--60) \\
PKS 1143$-$696 & \tablefootmark{*} & 48 $\pm$ 2 & 1.0 $\pm$ 0.1 & Sy1.2 & 0.244 & 1320.2 & 0.385 & 23 (0.1--2.4) \\
 & \tablefootmark{*} & [134 $\pm$ 7] & [2.4 $\pm$ 0.2] & & & & & 120 (2--10) \\
 & & & & & & & & 230 (17--60) \\
 & & & & & & & & 280 (20--100) \\
IGR J12107+3822 & \tablefootmark{*} & 109 $\pm$ 7 & 64.2 $\pm$ 1.9 & Sy1.5 & 0.0229 & 107.5 & 0.021 & 0.31 (0.2--12) \\
 & \tablefootmark{*} & [115 $\pm$ 7] & [68 $\pm$ 2] & & & & & 1.8 (14--150) \\
 & & & & & & & & 1.6 (17--60) \\
IGR J1248.2$-$5828 & \tablefootmark{*} & 1.1 $\pm$ 0.3 & 7.8 $\pm$ 0.5 & Sy1.9 & 0.028 & 131.9 & 0.624 & 0.85 (2--10) \\
 & \tablefootmark{*} & [5.8 $\pm$ 1.6] & [54 $\pm$ 4] & & & & & 1.6 (17--60) \\
 & & & & & & & & 2.1 (20--100) \\
IGR J13168$-$7157 & \tablefootmark{*} & 67 $\pm$ 10 & 47.1 $\pm$ 1.4 & Sy1.5 & 0.070 & 339.9 & 0.255 & 0.60 (0.1--2.4) \\
 & \tablefootmark{*} & [160 $\pm$ 20] & [103 $\pm$ 3] & & & & & 11 (0.2--12) \\
 & & & & & & & & 13 (17--60) \\
IGR J13187+0322 & --- & 17.2 $\pm$ 1.7 & 1.5 $\pm$ 0.3 & Type 1 & 0.6058 & 3846.2 & 0.031 & $<$540 (20--40) \\
 & --- & [17.2 $\pm$ 1.7] & [1.5 $\pm$ 0.3] & QSO & & & & $<$1300 (40--100) \\
Swift J1513.8$-$8125 & \tablefootmark{*} & 103 $\pm$ 5 & 37.3 $\pm$ 1.1 & Sy1.2 & 0.069 & 334.8 & 0.272 & 20 (14--150) \\
 & \tablefootmark{*} & [223 $\pm$ 11] & [83 $\pm$ 2] & & & & & 34 (14--195) \\
 & & & & & & & & 15 (17--60) \\
IGR J15311$-$3737 & --- & 48 $\pm$ 2 & 6.9 $\pm$ 0.3 & Sy1 & 0.127 & 640.8 & 0.320 & 2.3 (0.1--2.4) \\
 & --- & [120 $\pm$ 4] & [16.6 $\pm$ 0.5] & & & & & 12--16 (0.2--12) \\
 & & & & & & & & 44 (20--100) \\
IGR J18078+1123 & \tablefootmark{*} & 64 $\pm$ 4 & 12.6 $\pm$ 0.6 & Sy1/1.2 & 0.078 & 380.9 & 0.131 & 1.2 (0.1--2.4) \\
 & \tablefootmark{*} & [90 $\pm$ 6] & [18.6 $\pm$ 0.9] & & & & & 51 (17--60) \\
IGR J19077$-$3925 & \tablefootmark{*} & 4.8 $\pm$ 0.7 & 20.1 $\pm$ 1.2 & Sy1.9 & 0.0760 & 370.6 & 0.107 & 1.3 (0.1--2.4) \\
 & \tablefootmark{*} & [6.2 $\pm$ 0.9] & [28.0 $\pm$ 1.4] & & & & & 24 (20--100) \\
1RXS J191928.5$-$295808 & \tablefootmark{*} & 42 $\pm$ 8 & 122 $\pm$ 6 & Sy1.5/1.8 & 0.1669 & 863.5 & 0.139 & 12 (0.1--2.4) \\
 & \tablefootmark{*} & [56 $\pm$ 11] & [183 $\pm$ 9] & & & & & 120 (17--60) \\
 & & & & & & & & 67 (20--40) \\
 & & & & & & & & $<$42 (40--100) \\
1RXS J211928.4+333259 & \tablefootmark{*} & 10 $\pm$ 2 & 15.2 $\pm$ 0.8 & Sy1.5 & 0.051 & 244.4 & 0.217 & 0.44 (0.1--2.4) \\
 & \tablefootmark{*} & [18 $\pm$ 3] & [29.6 $\pm$ 1.5] & & & & & 6.8 (0.2--12) \\
 & & & & & & & & 5.6 (14--150) \\
 & & & & & & & & 11 (14--195) \\
 & & & & & & & & 9.1 (17--60) \\
 & & & & & & & & 11 (20--100) \\
1RXS J213944.3+595016 & \tablefootmark{*} & 3.0 $\pm$ 0.2 & 2.01 $\pm$ 0.10 & Sy1.5 & 0.114 & 570.4 & 1.271 & 1.7 (0.1--2.4) \\
 & \tablefootmark{*} & [112 $\pm$ 8] & [72 $\pm$ 4] & & & & & 23 (2--10) \\
 & & & & & & & & 14 (14--150) \\
 & & & & & & & & 40 (20--100) \\
IGR J22292+6647 & \tablefootmark{*} & 2.25 $\pm$ 0.11 & 1.24 $\pm$ 0.06 & Sy1.5 & 0.112 & 559.6 & 1.089 & 0.63 (0.1--2.4) \\
 & \tablefootmark{*} & [52 $\pm$ 3] & [26.3 $\pm$ 1.3] & & & & & 12 (0.2--12) \\
 & & & & & & & & 25 (2--10) \\
 & & & & & & & & 55 (14--150) \\
 & & & & & & & & 100 (14--195) \\
 & & & & & & & & 42 (17--60) \\
 & & & & & & & & 42 (20--100) \\
\hline
\end{tabular}}}
\tablefoot {Emission-line fluxes are reported both as observed and (between square brackets) corrected for the intervening Galactic absorption~\mbox{$E(B-V)_{\rm Gal}$} along the object line of sight (from Schlegel et~al. \cite{Schl98}). 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 in 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.  \\
\tablefoottext{*}{Heavily blended with [N~{\sc ii}]~lines.}}
\end{table}