\begin{table}%T4 
\par
  \caption{\label{lumi}\FUV, $U$, $B$, \Ha, $H$, \FIR, 15 $\mu$m, 60 $\mu$m, and 1.4~GHz luminosities for all galaxies analyzed in this work.} 
  \small%\centering
\par
  \begin{tabular}{lccccccccc }
 \hline\hline
   \noalign{\smallskip}
Galaxy &  $L_{\rm FUV}$ & $L_U$ & $L_B$ & $L_{\rm H\alpha}$ &  $L_H$  &$L_{\rm FIR}$ & $L_{\rm 15~ \mu m}$& $L_{\rm 60~ \mu m}$& $L_{\rm 1.4~ GHz}$ \\
   \noalign{\smallskip}
 & [10$^{39}$ \ergs~\AA$^{-1}$] & [10$^8$ \Lo] & [10$^8$ \Lo] &   [10$^{40}$ \ergs] & [10$^8$ \Lo] &[10$^{42}$ \ergs] & [10$^{22}$ W Hz$^{-1}$] &  
[10$^{23}$ W Hz$^{-1}$] & [10$^{20}$ W Hz$^{-1}$]\\ 
 \hline\noalign{\smallskip}
HCG 31       &  49~$\pm$~3    & 356   & 202~$\pm$~7  & 52~$\pm$~4     & 42.2  & 72~$\pm$~6\tablefootmark{a} &  3.9~$\pm$~0.7\tablefootmark{a}  &   14.1~$\pm$~1.1\tablefootmark{a} & 98~$\pm$~14\\
$''$ AC         & 24.9~$\pm$~1.5 &  175   &  92~$\pm$~4 & 36.3~$\pm$~2.3  &  18.0 &   \nodata	    &     \nodata    &	 \nodata   &   79~$\pm$~11 \\
$''$      B     & 11.0~$\pm$~0.9 &  73.8 & 47.4~$\pm$~1.8	&  3.1~$\pm$~0.3 & 10.0 &    \nodata	    &     \nodata    &	 \nodata   	  &    7.5~$\pm$~1.1 \\
$''$      E     & 1.51~$\pm$~0.12 &  6.3  & 3.13~$\pm$~0.17   & 1.49~$\pm$~0.16& 0.586 & \nodata &    \nodata        &	\nodata    	     &    \nodata \\
$''$      F\tablefootmark{b} & 1.52~$\pm$~0.15&  10.9 & 4.0~$\pm$~0.2   &    5.0~$\pm$~0.3 & 0.486 & \nodata&    \nodata        &	\nodata    	     &    \nodata \\
$''$      H     & 0.13~$\pm$~0.05 &  \nodata  &  \nodata   &    0.045~$\pm$~0.013 & \nodata & \nodata  &    \nodata        &	\nodata   &    \nodata \\
$''$      G     & 10.3~$\pm$~0.6 &  90.4 &  55~$\pm$~2	  &    6.4~$\pm$~0.4 & 13.1 &    \nodata  &   \nodata     &	 \nodata   	   &   11.9~$\pm$~1.8 \\
Mkn~1087     & \nodata & 1803   & 1127~$\pm$~83	  &   70~$\pm$~5   &   360 &   228~$\pm$~23   &   15~$\pm$~4    &   45~$\pm$~5	     &  178~$\pm$~9 \\
$''$ N          & \nodata & \nodata   &   26.1~$\pm$~0.9  &   2.27~$\pm$~0.19    &   5.01 &  \nodata &    \nodata        &	\nodata   &    \nodata \\
Haro~15      & 84~$\pm$~5 & 614   &  347~$\pm$~13	  &   42~$\pm$~5	 &   124 &   62~$\pm$~6   &    11~$\pm$~3    &   12.2~$\pm$~1.1      &  160~$\pm$~9 \\
Mkn~1199     & \nodata& 479   &  291~$\pm$~11	  &   49~$\pm$~7	     &   344 &  116~$\pm$~6   & 9.8~$\pm$~1.1   &   23.8~$\pm$~1.2      &  126~$\pm$~4 \\
$''$ NE         & \nodata & 21.1 & 16.6~$\pm$~0.6  & 0.90~$\pm$~0.23  &    21.7	 &     \nodata    &	\nodata   &   \nodata & \nodata \\
Mkn~5        & 0.274~$\pm$~0.018  & 4.21&   2.63~$\pm$~0.10  &  0.582~$\pm$~0.014  & 1.89 &  $<$0.30   &  $<$0.087  &0.036~$\pm$~0.007  &   3.9~$\pm$~0.8 \\
IRAS 08208+2816& 162~$\pm$~10 & 879  &  511~$\pm$~14 &  142~$\pm$~12	& 373 &  254~$\pm$~22  &  $<$5.5 	   &   49.7~$\pm$~4.0	   &  657~$\pm$~26 \\
IRAS 08339+6517& 79~$\pm$~4 &  1159  & 661~$\pm$~23	  &  120~$\pm$~6 &   592 &   198.6~$\pm$~1.8 &  18.3~$\pm$~1.8 &   42.6~$\pm$~0.3   &  249~$\pm$~37 \\
$''$ Comp.      &  1.17~$\pm$~0.10  &  38      & 29.9~$\pm$~1.6 &  2.1~$\pm$~0.4 &   23.3 & \nodata  &    \nodata    &	\nodata    	     &   \nodata   \\ 
POX 4        & 7.0~$\pm$~0.4 & 104.7 &   51.1~$\pm$~0.5  &  23.3~$\pm$~1.9\tablefootmark{c} &  17.9   &  6.9~$\pm$~0.5 &   $<$24  &	1.56~$\pm$~0.14    &   10.4~$\pm$~1.2 \\
$''$ Comp.      & 0.667~$\pm$~0.075 &  2.42 & 2.17~$\pm$~0.07 & 0.188~$\pm$~0.018\tablefootmark{c} & 1.1: & \nodata  &    \nodata    &	\nodata    	     &   \nodata   \\
UM 420       & 25.4~$\pm$~1.4 & 236   &  103~$\pm$~4	  &   47~$\pm$~3	& 57 &   142:	   &    \nodata        &	 27.7   	     &   74~$\pm$~34 \\
SBS 0926+606\tablefootmark{b} & 41.4~$\pm$~3.4 & 52.3  & 26.6~$\pm$~0.8  &  11.8~$\pm$~0.7 & 9.49  &    5.8~$\pm$~0.6    &    2.8  &	1.01~$\pm$~0.17    &   10~$\pm$~2 \\
$''$ A & 6.4~$\pm$~0.4 &  28.1  &  12.8~$\pm$~0.4	  &    9.4~$\pm$~0.5   &  3.63 &    \nodata	       &     \nodata    &	\nodata    	     &   \nodata \\
$''$ B &  35~$\pm$~3 &  24.2  & 13.8~$\pm$~0.4	  &    2.4~$\pm$~0.2     &   5.86 & \nodata	       &     \nodata    &	\nodata    	     &   \nodata \\
\par
SBS 0948+532 &\nodata&  121.3  &  36.7~$\pm$~1.0	  &   78~$\pm$~3	&  15.8 &   \nodata	       &     \nodata       &	\nodata    	     & $<$38 \\
SBS 1054+365 &0.090~$\pm$~0.006 & 0.982 &  0.655~$\pm$~0.018 & 0.450~$\pm$~0.017 & 0.413 & 0.23~$\pm$~0.03 & $<$0.042  & 0.041~$\pm$~0.005 & 0.098~$\pm$~0.011 \\
SBS 1211+540 &0.076~$\pm$~0.005 &  0.608  &  0.316~$\pm$~0.008  & 0.141~$\pm$~0.005   & 0.127 &  \nodata	 &   \nodata    &	 \nodata     & $<$0.50  \\
SBS 1319+579 & 0.86~$\pm$~0.05 &  63.1   &  40.2~$\pm$~1.4	  &    2.38~$\pm$~0.15  & 28.6 &    5.3:  &     \nodata       &	 0.85   	     & $<$2.9  \\
SBS 1415+437 & 0.409~$\pm$~0.023 &  1.69  &  1.00~$\pm$~0.03   &    0.50~$\pm$~0.02    & 0.581 &   \nodata &     \nodata     &	 \nodata  & $<$0.052  \\
III Zw 107   & \nodata & 286  & 177~$\pm$~5  &   40.1~$\pm$~1.8   & 77.3 &   50~$\pm$~8    &  $<$7.3 	   &   10.4~$\pm$~1.5      &   62~$\pm$~4 \\
Tol 9        & 9.5~$\pm$~0.7  & 118    & 79~$\pm$~2 &   22.9~$\pm$~1.6  &  55.5 &  35.4~$\pm$~1.6  &   2.5~$\pm$~0.7  &	6.1~$\pm$~0.5     &   87.3~$\pm$~1.6 \\
Tol 1457-262\tablefootmark{b}& 38.6~$\pm$~2.6 & 319  &  182~$\pm$~5	  &   63~$\pm$~3&  109    & 82~$\pm$~6   &  $<$6.5 	   &   17.2~$\pm$~1.1      &  216~$\pm$~10 \\
$''$ Obj~1      & 29.2~$\pm$~1.6 & 223 &   121~$\pm$~3 & 46.2~$\pm$~2.7  &  58.6 &   \nodata	       &     \nodata    &	\nodata    	     &   \nodata\\
$''$ Obj~2      & 9.2~$\pm$~1.1 &  97.3 &   60.3~$\pm$~1.7 & 17.2~$\pm$~0.8 &  45.3 &  \nodata	       &     \nodata    &	\nodata    	     &   \nodata\\
$''$ \#15       & 1.10~$\pm$~0.21 &  8.39 & 6.08~$\pm$~0.23 & 0.47~$\pm$~0.04 & 5.5: &    \nodata	   &     \nodata    &	\nodata    	     &   \nodata\\
Arp 252\tablefootmark{b} & 47.4~$\pm$~3.3 & 711    & 435~$\pm$~13 &   90~$\pm$~6	& 423   &  361~$\pm$~19      &   38~$\pm$~5    &   79~$\pm$~4	     & 1968~$\pm$~60 \\
$''$ ESO 566-8   & 38.5~$\pm$~2.7 & 597 & 350~$\pm$~10	 &   84~$\pm$~6	 &  313   & \nodata	       &     \nodata    &	\nodata    	     &   \nodata    \\
$''$ ESO 566-7   & 8.9~$\pm$~0.6  &  114 & 85~$\pm$~3	 &   6.3~$\pm$~0.4 &  110   &  \nodata	       &     \nodata    &	\nodata     &   \nodata     \\
NGC 5253    & 2.35~$\pm$~0.15 & 36.6   &  22.9~$\pm$~0.2 &  4.4~$\pm$~0.2&  14.2   & 2.583~$\pm$~0.009  & 0.479~$\pm$~0.004 &  0.571~$\pm$~0.001  &   1.47~$\pm$~0.06 \\
\hline
  \end{tabular}
\tablefoot{\tablefoottext{a}{As IRAS data do not allow to be distinguished regions within the HCG~31 group, this value considers the flux of all galaxy members.}\\
  \tablefoottext{b}{We are considering the flux of two galaxies: members F1 and F2 for HCG~31~F; galaxies~A and B for SBS~0926+606; \emph{obj~1} and \emph{obj~2}  
for Tol~1457-262; and ESO~566-8 (A) and ESO~566-7 (B) for Arp 252.}\\
  \tablefoottext{c}{As we pointed out in Paper~I, the \Ha\ flux for POX~4 provided by  M\'endez \& Esteban (\cite{endez1999}) seems to be overestimated, so we consider here the value  
provided by  Gil~de~Paz et~al. (\cite{Gil2003}), which is 0.61 times smaller. We also scale our \Ha\ flux of POX~4~Comp using this factor. }}
\vspace*{4.5mm}
\end{table}