\begin{table}%t1
\caption{\label{TableSample}Main characteristics of the sample of ULIRGs. The galaxies are sorted by decreasing nuclear distance.} 
\small%\centerline
{
\begin{tabular}{lcccccccc}       
\hline
\hline
\noalign{\smallskip}
IRAS Name &RA(J2000) & Dec(J2000) & Spectral Class & \textit{z} & $D_{\rm{L}}$$^a$ & ${\log(L_{\rm{IR}})}$$^b$ & Scale & Morphology$^c$ \\
 & (hh:mm:ss) & (deg:mm:ss) & (Optical) & & (Mpc) &(L$_{\odot}$) &(kpc arcsec$^{-1}$) & \\
\hline
IRAS~13156+0435      &              13:18:07.6 & +04:18:59.4 & H~{\sc ii}/LINER (G)& 0.113 & 525 & 12.13                & 2.058 & IP at 36.0~kpc \\
IRAS~13342+3932      &              13:36:23.3 & +39:16:41.9 & Sey1 (E)             & 0.179 & 866 & 12.51                & 3.026 & IP at 25.1~kpc  \\
IRAS~18580+6527      &              18:58:06.3 & +65:31:32.2 & H~{\sc ii}/Sey2 (G) & 0.176 & 850 & 12.26   & 2.986 & IP at 15.0~kpc 	      \\
IRAS~16007+3743   &              16:02:36.9 & +37:34:39.7 & LINER (H)            & 0.185 & 898 & 12.11                & 3.100 & IP at 14.2~kpc	      \\
IRAS~06268+3509      &              06:30:12.6 & +35:07:51.9 & H~{\sc ii} (C)$^d$      & 0.169 & 813 & 12.51$^e$   & 2.895 & IP at 9.1~kpc \\
IRAS~08572+3915      &              09:00:25.4 & +39:03:54.4 & LINER (E)$^f$           & 0.058 & 259 & 12.17                & 1.130 & IP at 6.1~kpc \\
IRAS~14348-1447   &              14:37:38.4 & --15:00:22.8 & LINER (E)            & 0.083 & 378 & 12.39                & 1.556 & IP at 5.5~kpc 	      \\
Arp~299$^g$ & 11:28:30.4 & +58:34:10.0 & H~{\sc ii}/Sey2 (D)$^h$ & 0.010 & 43  & 11.81                & 0.205 & IP at 5.0~kpc  \\   
IRAS~13469+5833      &              13:48:40.3 & +58:18:50.0 & H~{\sc ii}  (I)$^i$     & 0.158 & 755 & 12.31                & 2.726 & IP at 4.5~kpc    \\
IRAS~12112+0305               &12:13:42.9 & +02:48:29.0 & LINER (E)            & 0.073 & 330 & 12.37                & 1.395 & IP at 4.0~kpc  \\
Mrk~463     & 13:56:02.8 & +18:22:17.2 & Sey1/Sey2 (F, G)$^j$     & 0.050 & 222 & 11.81                & 0.984 & DN at 3.8~kpc    \\
IRAS~06487+2208      &              06:51:45.7 & +22:04:27.0 & H~{\sc ii} (C)      & 0.144 & 682 & 12.57$^k$ & 2.522 & DN at 1.5~kpc \\
IRAS~11087+5351      &              11:11:36.4 & +53:35:02.0 & Sey1 (G)             & 0.143 & 677 & 12.13                & 2.507 & DN at 1.5~kpc  \\
Mrk~273     & 13:44:42.0 & +55:53:12.1 & LINER/Sey2 (B, E)$^l$    & 0.038 & 167 & 12.18                & 0.749 & DN at 0.7~kpc    \\
Arp~220     & 15:34:57.1 & +23:30:11.5 & LINER (E)            & 0.018 & 78  & 12.20                & 0.368 & DN at 0.4~kpc	      \\ 
IRAS~17208-0014   &              17:23:21.9 & --00:17:00.9 & LINER (A)$^m$           & 0.043 & 190 & 12.43                & 0.844 & SN 	      \\
IRAS~15250+3609   &              15:26:59.4 & +35:58:37.5 & LINER (H)$^n$            & 0.055 & 245 & 12.09                & 1.072 & SN 	      \\
IRAS~12490-1009      &              12:51:40.7 & --10:25:26.1 & H~{\sc ii}/LINER (G)& 0.101 & 465 & 12.07                & 1.854 & SN  \\
IRAS~14060+2919      &              14:08:18.9 & +29:04:46.9 & H~{\sc ii}  (E)     & 0.117 & 545 & 12.18                & 2.113 & SN    \\
IRAS~09427+1929     &              09:45:32.4 & +19:15:34.9 & H~{\sc ii} (H)      & 0.149 & 708 & 12.10                & 2.600 & SN \\
IRAS~15206+3342   &             15:22:38.0 & +33:31:35.9 & H~{\sc ii} (E)      & 0.124 & 580 & 12.27                & 2.232 & SN 	      \\
Mrk~231     & 12:56:14.2 & +56:52:25.2 & Sey1 (E)             & 0.042 & 186 & 12.57                & 0.832 & SN  \\
\hline                                   
\end{tabular} }
\smallskip 
$^a$ {For the luminosity distances, the Wright (\cite{Wright2006}) cosmology calculator has been used.}\\
$^b$ {$L_{\rm IR} (8{-}1000~\mu$m) was derived following Sanders \& Mirabel (\cite{Sanders1996}) ($L(8{-}1000~\mu {\rm m})=4\pi {D_{\rm L}}^{2}F_{\rm IR}[L_{\odot}]$, with $F_{\rm FIR}=1.26\times 10^{-14}\times(2.58f_{60}+f_{100})[{\rm Wm}^{-2}]$. The quantities $f_{12}$, $f_{25}$, $f_{60}$, and $f_{100}$ are the \textit{IRAS} flux densities in~Jy at~12, 25, 60 and~100~$\mu$m.). The IRAS fluxes were obtained from the IRAS Faint Galaxy Sample (Moshir et~al. \cite{Moshir1993}, Vizier on line catalogue II/156A).}\\
$^c$ {IP means interacting pair, DN double nucleus and SN single nucleus. The distances in kpc represent the projected nuclear distance as measured in the {F814W} HST image.}\\
$^d$ {(C) Darling \& Giovanelli (\cite{Darling2006}).}\\
$^e$ {IRAS fluxes obtained from the IRAS point Source Catalogue.}\\
$^f$ {(E) Kim et~al. (\cite{Kim1998}).}\\
$^g$ {Arp~299 is the system formed by NGC~3690 (to the east) and IC~694 (to the west).}\\
$^h$ {(D) Garc\'{\i}a-Mar\'{\i}n et~al. (\cite{Garc2006}).}\\
$^i$ {Veilleux et~al. (\cite{Veilleux1999}).}\\
 $^j$ {(F) Miller \& Goodrich (\cite{Miller1990}); (G) Garc\'{\i}a-Mar\'{\i}n (\cite{Garc2007}).}\\
 $^k$ {IRAS fluxes obtained from the IRAS point Source Catalogue.}\\
 $^l$ {(B) Colina et~al. (\cite{Colina1999}).}\\
 $^m$ {(A) Arribas \& Colina (\cite{Arribas2003}).}\\
 $^n$ {(H) Veilleux et~al. (\cite{Veilleux1995}).}
\end{table}