\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}