\begin{table}%t1
\caption{\label{Table1}Extinction and structural properties for the sample of galaxies.}
%\centerline
 {\small \begin{tabular}{lccccccccccc}
 \hline \hline\noalign{\smallskip}
Galaxy$^a$ &log({$L_{\rm{IR}}$})$^b$ & \textit{z} & {$A_{\rm{V}}$$_{\rm{median}}$}$^c$ & {$A_{\rm{V}}$$_{\rm{nuc}}$}$^d$ & {{$A_{\rm{V}}$$_{\rm{max}}$}}$^e$ &Sep$^f$ & Scale & {{$R_{\rm{eff}}$}}(optical) & {{$R_{\rm{eff}}$}}$^g$ & {{$R_{\rm{eff}}$}}$^h$ & Morphology$^i$ \\ 
& {{$L_{\odot}$}} & & (mag) & (mag)   &(mag) & (kpc) & (kpc/arcsec) & (kpc) & (kpc) & (kpc) & \\
\hline
IRAS~13156+0435N   &12.13 & 0.113 &  2.5  $\pm$  0.8  & 3.3 & 3.7 & 3.9  $\pm$  1.0 & 2.058  &  & 5.9 &  &  IP at 36.0~kpc\\
IRAS~13156+0435S   &   &   &  0.9  $\pm$  0.4  & 1.5 & 1.7 & 2.2  $\pm$ 1.0 & 2.058  &   & 4.9 &   &   \\
IRAS~18580+6527E   &12.26 &0.176 &  1.3  $\pm$  0.8  & 0.5 & 3.9 & 20.3 $\pm$ 1.5 & 2.986  & 11.3$^j$& 6.5 &    &  IP at 15.0~kpc\\
IRAS~18580+6527W   &   &      &   & 0.8 & 3.9 & 8.7  $\pm$ 1.5 & 2.986  & 9.4$^{j}$  & 4.3 & &  \\
IRAS~16007+3743E   &12.11 & 0.185 &  1.9  $\pm$  1.0  & 4.5 & 5.0 & 12.7 $\pm$ 1.5 & 3.100  &  & 4.0 & &  IP at 14.2~kpc\\
IRAS~16007+3743W   &  & &  & 4.7 & 5.0 & 1.4  $\pm$  1.5 & 3.100  &                     & 4.2 & &                \\
IRAS~06268+3509N   &12.51 &0.169 &  2.0  $\pm$  1.2  & 5.7 & 6.9 & 3.2  $\pm$ 1.4 & 2.895  & 8.3$^{j}$           & 2.0 & 2.1       & IP at 9.1~kpc \\
IRAS~06268+3509S   &      &      &               & 2.2 & 6.9 & 10.5 $\pm$ 1.4 & 2.895  & 6.3$^{j}$           & 1.5 & 1.1       &                \\
IRAS~08572+3915N   &12.17 &0.058 &  1.7  $\pm$  1.1  & 2.3 & 5.8 & 0.0  $\pm$ 0.6 & 1.130  & 2.9$^k$                 & 2.8 & 0.6  &IP at 6.1~kpc \\
IRAS~08572+3915S   &      &      &               & 0.4 & 5.8 & 1.3  $\pm$ 0.6 & 1.130  & 4.3$^{k}$           & 1.4 & 0.6  &              \\
IRAS~14348$-$1447N &12.39 &0.083 &  2.9 $\pm$ 1.0  & 5.4 & 5.8 & 5.6  $\pm$ 0.8 & 1.556  & 5.3$^l$                & 1.4 & 1.5  &IP at 5.5~kpc \\
IRAS~14348$-$1447S &      &      &               & 4.1 & 5.8 & 0.8  $\pm$ 0.8 & 1.556  & 4.1$^{l}$           & 3.0 & 1.3  &                \\
Arp~299/NGC~3690   &11.81 &0.010 &  1.9 $\pm$ 0.6  & 3.7 & 4.3 & 0.5  $\pm$ 0.1 & 0.205  &                     & 1.2 & 0.9  &  IP at 5.0~kpc \\
Arp~299/IC~694     &      &      &  2.0 $\pm$ 0.6  & 2.7 & 3.4 & 0.3  $\pm$ 0.1 & 0.205  &                     & 2.0 & 0.4  &                \\
IRAS~12112+0305N   &12.37 &0.073 &  1.7 $\pm$ 1.3  & 3.0 & 7.7 & 5.5  $\pm$ 0.7 & 1.395  & 3.3$^{l}$           & 2.0 & 1.7  &  IP at 4.0~kpc \\
IRAS~12112+0305S   &      &      &               & 7.7 & 7.7 & 0.0  $\pm$ 0.7 & 1.395  & 4.5$^{l}$           & 1.5 & 1.1  &                 \\
Mrk~463-E          &11.81 &0.050 &  0.9 $\pm$ 0.5  & 0.7 & 3.0 & 4.7  $\pm$ 0.5 & 0.984  &                     & 1.0 & 0.2  &  DN at 3.8~kpc \\
Mrk~463-W          &      &      &               & 1.5 & 3.0 & 8.4  $\pm$ 0.5 & 0.984  &                     & 1.0 & 1.0  &                \\
IRAS~06487+2208    &12.57 &0.144 &  2.2 $\pm$ 0.6  & 2.4 & 3.5 & 4.3  $\pm$ 0.6 & 2.522  &                     & 1.5 & &  DN at 1.5~kpc \\
IRAS~11087+5351    &12.13 &0.143 &  1.2 $\pm$ 1.0  & 3.0 & 3.0 & 0.0  $\pm$ 0.6 & 2.507  &                     & 8.9 & &  DN at 1.5~kpc \\
Mrk~273            &12.18 &0.038 &  1.9 $\pm$ 1.0  & 3.1 & 4.9 & 2.1  $\pm$ 0.4 & 0.749  & 4.3$^{l}$           & 4.4 & 2.0  &  DN at 0.7~kpc \\
IRAS~17208$-$0014  &12.43 &0.043 &  5.5 $\pm$ 2.6  & 5.0 & 9.0 & 0.8  $\pm$ 0.4 & 0.844  & 3.6$^{l}$           & 3.2 & 1.5  &  SN            \\
IRAS~15250+3609    &12.09 &0.055 &  2.3 $\pm$ 1.7  & 2.5 & 7.9 & 2.4  $\pm$ 0.5 & 1.072  & 2.2$^{l}$           & 1.9 & 1.4  &  SN            \\
IRAS~12490$-$1009  &12.07 &0.101 &  1.3 $\pm$ 0.7  & 1.1 & 3.3 & 3.6  $\pm$ 0.9 & 1.854  &                     & 7.6 & &  SN            \\
IRAS~14060+2919    &12.18 &0.117 &  1.5 $\pm$ 0.5  & 2.2 & 2.5 & 2.3  $\pm$ 1.0 & 2.113  &                     & 4.8 & &  SN            \\
IRAS~15206+3342    &12.27 &0.124 &  0.8 $\pm$ 0.5  & 1.0 & 2.0 & 2.4  $\pm$ 1.0 & 2.232  & 2.2$^{k}$           & 2.9 &      &  SN            \\
\hline                                  
\end{tabular}}
\medskip
$^a$ The galaxies are listed according to decreasing nuclear separation (see Garc\'{\i}a-Mar\'{\i}n et~al. \cite{Garcia2009}); $^b$~$L_{\rm{IR}}$ (8--1000~$\mu$m) was derived following Sanders \& Mirabel \cite{Sanders1996}); $^c$~median extinction of the entire system with the deviation that effectively represents the distribution of the extinction values over the entire area where the H$\alpha$ and H$\beta$ measurements can be obtained. For pre-coalescence systems with one pointing per nuclei, the median has been calculated for each pointing; $^d$~nuclear extinction of the galaxy. The uncertainties are about~20\%; $^e$~maximum extinction of the system; $^f$~separation between the optical nucleus, identified as the peak position in the $F814W$ band of the HST images, and the position of the peak of extinction; $^g$~effective radius measured from the HST~WFPC2 camera, with the filter~$F814W$, corresponding to a central wavelength of 0.82~$\mu$m and a filter width of 0.17~$\mu$m; $^h$~effective radius measured from the HST NICMOS2 camera, with the filter~$F160W$, corresponding to a central wavelength of 1.55~$\mu$m and a filter width of 0.40~$\mu$m; $^i$  IP~means interacting pair, DN double nucleus and SN single nucleus; $^j$ effective radius measured from the HST WFPC2 camera, with the filter~$F606W$, corresponding to a central wavelength of 0.58~$\mu$m, and a filter width of 0.16~$\mu$m; $^k$~effective radius measured from the HST~WFPC2 camera, with the filter~$F439W$, corresponding to a central wavelength of 0.43~$\mu$m and a filter width of 0.05~$\mu$m; $^l$~effective radius measured from the HST ACS camera, with the filter~$F435W$, corresponding to a central wavelength of 0.43~$\mu$m and a filter width of 0.14~$\mu$m.
\end{table}