\begin{table}%t3
\caption{\label{tab3}Synoptic table containing the main results concerning the 6~X-ray binaries (see Fig.~\ref{fig7}) identified in the present sample of {\it INTEGRAL} sources.}
\par
%\centering
\par
 {  {
\begin{tabular}{lccccccccccr}
\hline
\hline
\noalign{\smallskip}
\multicolumn{1}{c}{Object} & \multicolumn{2}{c}{H$_\alpha$} & 
\multicolumn{2}{c}{H$_\beta$} &
\multicolumn{2}{c}{He {\sc ii} $\lambda$4686} &
Optical & $A_V$ & $d$ & Spectral & \multicolumn{1}{c}{$L_{\rm X}$} \\
 & {\it EW} & Flux & {\it EW} & Flux & {\it EW} & Flux & mag & (mag) & (kpc) & type & \\
\hline\noalign{\smallskip}
IGR J01054$-$7253 & 7.15 $\pm$ 0.15 & 16.8 $\pm$ 0.3 & 0.47 $\pm$ 0.12 & 2.0 $\pm$ 0.5 & in abs. & in abs. &
 14.81\tablefootmark{a} ($V$) & $\sim$0.7 & 60\tablefootmark{b} & B0~III & 0.13 (0.1--2.4) \\
 & & & & & & & & & & & 700\tablefootmark{c} (3--10) \\
 & & & & & & & & & & & 77 (20--100) \\
Swift J0208.4$-$7428 & 2.9 $\pm$ 0.3 & 4.5 $\pm$ 0.5 & in abs. & in abs. & $<$0.5 & $<$0.2 &
 14.75\tablefootmark{d} ($V$) & 0.18\tablefootmark{e} & 60\tablefootmark{b} & B1~III & 19 (0.2--12) \\
 & & & & & & & & & & & 6.5 (3--10) \\
 & & & & & & & & & & & 108 (15--35) \\
IGR J08262$-$3736 & 65 $\pm$ 2 & 1050 $\pm$ 30 & 5.5 $\pm$ 0.4 & 96 $\pm$ 7 & in abs.? & in abs.? &
 12.9\tablefootmark{f} ($V$) & $\sim$3.3\tablefootmark{e} & $\sim$6.1 & OB V & 0.43 (20--100) \\
IGR J16327$-$4940 & 31.3 $\pm$ 0.9 & 370 $\pm$ 11 & 7.6 $\pm$ 0.7 & 3.8 $\pm$ 0.4 & in abs. & in abs. &
 15.5 ($R$) & 11.2 & $\approx$2 & OB giant & $<$0.0072 (20--40) \\
 & & & & & & & & & & & 0.018 (40--100) \\
IGR J19113+1533 & 22.5 $\pm$ 1.1 & 159 $\pm$ 8 & 3.6 $\pm$ 0.7 & 5.9 $\pm$ 1.2 & $<$1.2 & $<$1.5 &
 13.3 ($R$) & 7.0 & $\sim$9.1 & sgB[e] & $<$0.15 (20--40) \\
 & & & & & & & & & & & $<$0.28 (40--100) \\
\hline\noalign{\smallskip} 
IGR J16287$-$5021 & 52 $\pm$ 3 & 1.75 $\pm$ 0.09 & 19 $\pm$ 6 & 0.23 $\pm$ 0.07 & 15 $\pm$ 5 & 0.16 $\pm$ 0.05 &
 19.5\tablefootmark{g} ($R$) & 3.1 & $<$19 & --- & $<$1.3 (0.2--12) \\
 & & & & & & & & & & & $<$2.9 (0.3--10) \\
 & & & & & & & & & & & $<$2.8 (2--10) \\
 & & & & & & & & & & & $<$3.8 (17--60) \\
 & & & & & & & & & & & $<$2.3 (20--40) \\
 & & & & & & & & & & & $<$1.2 (40--100) \\
\hline
\end{tabular}}}
\tablefoot {{\it EW}s are expressed in \AA, line fluxes are in units of 10$^{-15}$~erg~cm$^{-2}$~s$^{-1}$, whereas X-ray luminosities are in units of 10$^{35}$~erg~s$^{-1}$ and the reference band (between round brackets) is expressed in~keV. \\
\tablefoottext{a}{From Massey (\cite{Mass02});}
\tablefoottext{b}{from Harries et~al. (\cite{Harr03});}
\tablefoottext{c}{from Coe et~al. (\cite{Coe10});}
\tablefoottext{d}{from Demers \& Irwin (\cite{Deme91});}
\tablefoottext{e}{only the Galactic reddening along the line of sight was assumed;}
\tablefoottext{f}{from Pettersson (\cite{Pett87});}
\tablefoottext{g}{this work.}}
%\vspace*{2mm}
\end{table}