\begin{table}%T5 
\par
  \caption{\label{sfrg}\SFR\ values (in units of~\Moy) derived for each galaxy using different luminosities and calibrations.} 
 \small%\centering
\par
  \begin{tabular}{l c cc  ccccccc}
  \hline\hline
   \noalign{\smallskip}
Galaxy    & $FUV$  & $U$ & \multicolumn{2}{c}{$B$} &     \Ha   &   FIR &  15 $\mu$m &  60 $\mu$m    &  1.4 GHz &   Assumed  \\
\cline{4-5}
\noalign{\smallskip}
        &S07   & Eq.~(\ref{sfru})  &   G84   &  Eq.~(\ref{sfrb})  &   K98   &  K98  &  R01       &  C92          &  C02       & \SFR \\
\hline
HCG 31   & 4.0~$\pm$~0.3 & 2.8 & 0.59 & 2.5 &  4.1~$\pm$~0.4 &   3.3~$\pm$~0.3 & 1.2~$\pm$~0.2 & 2.8~$\pm$~0.2 & 2.5~$\pm$~0.2 & 3.1 \\ 
   $''$ AC (NGC~1741)  & 2.02~$\pm$~0.12 & 1.5 & 0.27  & 1.2  &  2.88~$\pm$~0.18 &  \nodata & \nodata  &  \nodata  & 1.98~$\pm$~0.03  & 2.0 \\  
  $''$ B  & 0.89~$\pm$~0.07 & 0.68 &  0.14  & 0.67  &  0.24~$\pm$~0.02 & \nodata & \nodata  &  \nodata    &	 0.19~$\pm$~0.03    & 0.62 \\ 
  $''$ E  & 0.122~$\pm$~0.009 & 0.073 &  0.009 & 0.057   &  0.118~$\pm$~0.013  & \nodata & \nodata  &  \nodata  & \nodata & 0.10 \\  
  $''$ F  & 0.123~$\pm$~0.013 & 0.12 & 0.012 & 0.071  &  0.40~$\pm$~0.03 & \nodata & 	\nodata    &    \nodata	    &\nodata    &  0.20 \\  
  $''$ G (Mkn~1090) & 0.83~$\pm$~0.05 & 0.81 & 0.16  & 0.77  &  0.51~$\pm$~0.03 & \nodata & 	\nodata  &  \nodata	 &  0.30~$\pm$~0.04  & 0.49 \\  
  $''$ H  & 0.011~$\pm$~0.004 & \nodata & \nodata  & \nodata  & 0.004~$\pm$~0.001 & \nodata & 	\nodata    &      \nodata	    &\nodata  & 0.008 \\
Mkn 1087 &\nodata & 12.1  & 3.27  & 11.8  &   5.6~$\pm$~0.4  & 10.3~$\pm$~1.1 & 4.6~$\pm$~1.3 & 8.8~$\pm$~1.0 & 4.5~$\pm$~0.2     & 6.3   \\
$''$ N   & \nodata & \nodata & 0.076 & 0.39 & 0.180~$\pm$~0.015  & \nodata & \nodata &\nodata & \nodata & 0.12 \\
Haro 15  &6.8~$\pm$~0.4 & 4.6 &  1.00  &  4.1  &   3.3~$\pm$~0.4  &  2.8~$\pm$~0.3 & 3.2~$\pm$~0.9 & 2.4~$\pm$~0.2 & 4.0~$\pm$~0.2   & 3.6 \\ 
Mkn 1199 &\nodata & 3.7 &  0.84  &  3.5  &   3.9~$\pm$~0.6  &	 5.2~$\pm$~0.3 & 3.0~$\pm$~0.3 & 4.7~$\pm$~0.2 & 3.16~$\pm$~0.10    & 3.7 \\ 
$''$ NE     & \nodata& 0.22  & 0.048  &  0.26  &   0.07~$\pm$~0.02 & \nodata & 	\nodata    &      \nodata	    & \nodata  & 0.05 \\
Mkn 5    & 0.0222~$\pm$~0.0014 & 0.050 & 0.008 & 0.049 & 0.046~$\pm$~0.011&	$<$0.014  &	$<$0.03   &  0.067~$\pm$~0.008  &  $<$0.10  & 0.040 \\ 
IRAS~08208+2816& 13.1~$\pm$~0.8 & 6.4 & 1.48& 5.8 &  11.3~$\pm$~0.9  &	11.4~$\pm$~1.0 &$<$1.68 &   9.7~$\pm$~0.8   &  16.4~$\pm$~0.7  & 11.6 \\ 
IRAS~08339+6517& 6.4~$\pm$~0.4  & 8.2 & 1.92& 7.3 &  9.5~$\pm$~0.5  & 8.93~$\pm$~0.08& 5.6 $\pm$ 0.6 &  8.36 $\pm$ 0.06 &  6.2~$\pm$~0.9  & 7.0 \\  
$''$ Comp          & 0.095~$\pm$~0.008 & 0.37  & 0.087 &  0.44  & 0.17~$\pm$~0.02  & \nodata & 	\nodata    &      \nodata	    &\nodata  & 0.10 \\
POX 4   & 0.57~$\pm$~0.03 & 0.93 & 0.15 & 0.72  &  1.85~$\pm$~0.06 & 0.31~$\pm$~0.02 &$<$7.48 &  0.31~$\pm$~0.03 &  0.26~$\pm$~0.03 &  0.54 \\ 
$''$ Comp  &0.054~$\pm$~0.006 & 0.030 & 0.0063 & 0.041 & 0.012~$\pm$~0.004 & \nodata & 	\nodata    &   \nodata	 &\nodata & 0.031 \\  
UM 420  & 2.01~$\pm$~0.11 & 1.9 & 0.30  &  1.4  &  3.7~$\pm$~0.2  &	6.4	   &	\nodata   &  5.4	 &    1.9~$\pm$~0.8   &  2.1 \\  
SBS~0926+606 &  3.4~$\pm$~0.3 & 0.50 & 0.08  & 0.40 &  0.94~$\pm$~0.06 & 0.26~$\pm$~0.03 &$<$0.86  &    0.20~$\pm$~0.03 &  0.25~$\pm$~0.06 & 0.95 \\  
      $''$ A & 0.53~$\pm$~0.03 & 0.28  &  0.04 & 0.20 &  0.75~$\pm$~0.04 & \nodata  &	\nodata    &     \nodata	&    \nodata  & 0.52 \\  
      $''$ B & 2.82~$\pm$~0.25 & 0.25 &  0.04 & 0.22 &  0.19~$\pm$~0.02 & \nodata  &	\nodata  &    \nodata	&    \nodata     &      1.4?   \\
\par
SBS~0948+532 & \nodata & 1.1 & 0.11  & 0.53 &  6.2~$\pm$~0.2  & \nodata  &	\nodata     &    \nodata  &    $<$0.95       & 4.2 \\ 
SBS~1054+365 & 0.0073~$\pm$~0.0005 & 0.013 & 0.0014& 0.019& 0.036~$\pm$~0.001&  0.016 &	$<$0.01  &   0.015  &  0.025~$\pm$~0.004  & 0.018 \\  
SBS~1211+540 & 0.0062~$\pm$~0.0004 & 0.009 & 0.0007& 0.009& 0.011~$\pm$~0.001& \nodata &  \nodata  &   \nodata  &    $<$0.01  & 0.007 \\ 
SBS~1319+579 & 0.069~$\pm$~0.004   & 0.59 & 0.12  & 0.58 & 0.189~$\pm$~0.012 &  0.24	 &	  \nodata   &    0.17  &  $<$0.07  & 0.15 \\  
SBS~1415+437 & 0.0331~$\pm$~0.0018 & 0.022 & 0.0029& 0.020& 0.039~$\pm$~0.002 & \nodata& \nodata  &  \nodata &    $<$0.01  & 0.030 \\  
III~Zw~107   & \nodata & 2.3 & 0.51  & 2.2  &  3.19~$\pm$~0.15 &  2.3~$\pm$~0.4  & $<$2.24 &  2.0~$\pm$~0.3  &  1.52~$\pm$~0.09  & 2.0 \\  
Tol 9        & 0.77~$\pm$~0.06 & 1.0 & 0.23 & 1.1 &  1.82~$\pm$~0.13 & 1.59~$\pm$~0.07 &0.8~$\pm$~0.2& 1.19~$\pm$~0.08& 2.18~$\pm$~0.04 & 1.3 \\  
Tol 1457-262 &  3.2~$\pm$~0.2 & 2.6 & 0.53  & 2.3  &  5.0~$\pm$~0.3  & 3.7~$\pm$~0.3   &	$<$1.99   &   3.4~$\pm$~0.2 & 5.4~$\pm$~0.3 & 3.8 \\ 
     $''$ Obj~1 & 2.37~$\pm$~0.13 & 1.8 & 0.35 & 1.6 &   3.7~$\pm$~0.2 & \nodata&	   \nodata     &     \nodata &  \nodata & 2.4 \\  
    $''$  Obj~2 & 0.74~$\pm$~0.09 & 0.87  & 0.17 & 0.83 &   1.37~$\pm$~0.06 & \nodata&	   \nodata   &     \nodata	 &  \nodata & 0.83 \\ 
	 $''$  \#15 & 0.089~$\pm$~0.017& 0.09 & 0.018 & 0.10 & 0.038~$\pm$~0.003 & \nodata & \nodata&	   \nodata     &     \nodata & 0.06 \\  
Arp 252      & 3.84~$\pm$~0.26 & 5.3 & 1.26  & 5.0  &  7.2~$\pm$~0.5  & 16.2~$\pm$~0.9 & 11.6~$\pm$~1.4 & 15.4~$\pm$~0.8 & 49.2~$\pm$~1.5  & 10 \\			 
    $''$ ESO 566-8 & 3.12~$\pm$~0.22 & 4.5 & 1.01 & 4.1  &  6.7~$\pm$~0.5 & \nodata&	   \nodata     &   \nodata	  & \nodata & 3.8 \\ 
    $''$ ESO 566-7 & 0.72~$\pm$~0.04 & 1.0 & 0.25 & 1.1 & 0.50~$\pm$~0.04  &  \nodata&	   \nodata     &   \nodata	  & \nodata &  0.53 \\  
NGC 5253    &  0.190~$\pm$~0.010  & 0.36 & 0.07 & 0.35 &  0.348~$\pm$~0.017 & 0.12  &	0.15  &    0.11    &    0.037~$\pm$~0.002  & 0.14 \\ 
\hline
  \end{tabular}
  \tablebib{S07 =  Salim et~al. (\cite{Salim2007}); G84 =  Gallagher et~al. (\cite{Gallagher1984}); K98 =  Kennicutt (\cite{Kennicutt1998});  R01 =  Roussel et~al. (\cite{Roussel2001}); C92 =  Condon (\cite{Condon1992}); C02 =  Condon et~al. (\cite{Condon2002}) using the  
expression for $M>5$~\Mo. }
\end{table}