\begin{table}%t6
\par
\caption{\label{tab-lum}Source luminosities  calculated from the integrated "normal-galaxy'' spectrum (Lagache Lum.), 
Stickel's formula (Stickel Lum.) and the best fit Dale spectrum (Dale Lum.) with 
its $\alpha$~value. The H$\alpha$~luminosities, uncorrected for 
extinction (hence the "$>$'' sign in the corresponding~SFR), are also given. 
The $K$~luminosity is directly derived from the $K$~magnitude. 
The~"$q$'' parameter is the logarithmic ratio of~IR to radio flux, following 
\citet{helou85}. } 
%\centerline
{
\begin{tabular}{cccccccccc}
 \hline \hline
ID& $z$& Lagache Lum.& Stickel L.&  Dale L. (and $\alpha$)& H$\alpha$ L.& $K$ Lum.& {\rm SFR}(IR)& {\rm SFR}(H$\alpha$)& $q$\\ 
& & ($10^{10}~L_{\odot}$)&($10^{10}~L_{\odot}$)& ( $10^{10} L_{\odot}$)& ($10^{6}~L_{\odot}$)&($10^{9}~L_{\odot}$) &$ M_{\odot}/$yr$^{-1}$& $10^{-2}~M_{\odot}~$yr$^{-1}$& \\ \hline
     0  &  0.145  &  52.3   &73.0&  95.3 (1.69)&  222& 5.87    &  68& $>$675& 2.30\\ 
     1  &  0.030  &   1.5   & 1.3&   1.8 (1.83)&  4.9& 0.70    & 1.9&  $>$15& 2.69\\ 
     2  &  0.063  &   6.4   &4.6 &   6.1 (2.07)&  3.2& 2.32    & 8.3& $>$9.7& 2.60\\ 
     3  &  0.063  &   4.9   &    &             &  5.2& 2.54    & 6.4&  $>$16&     \\ 
     4  &  0.063  &   4.6   &3.4 &   5.2 (2.52)&  2.2& 4.97    & 6.0& $>$6.7& 2.32\\ 
     5  &  0.288  & 100.8   &70.5& 113.6 (2.35)&     &         & 131&       &     \\ 
     6  &  0.073  &   5.6   &4.4 &   7.2 (2.52)& 11.3& 2.80    & 7.3&  $>$34&     \\ 
     7  &  0.063  &   3.6   &3.8 &             & 12.8& 2.14    & 4.7&  $>$39& 2.35\\ 
     9  &  0.053  &   2.4   &    &             &  2.8& 3.14    & 3.1& $>$8.5&     \\ 
     11 &  0.063  &   3.6   &    &             &  3.0& 1.39    & 4.7& $>$9.1&     \\ 
     12 &  0.063  &   3.8   &    &             &  8.2& 0.93    & 4.9&  $>$25& 2.66\\ 
     14 &  0.07   &   4.1   &4.8 &   7.9 (2.25)&     &         & 5.3&       &     \\ 
     15 &  0.23   &  48.6   &    &             &     & 4.23    &  63&       &     \\ 
     16 &  0.090  &   6.8   &8.5 &  13.3 (2.13)& 23.6& 3.02    & 8.8&  $>$72& 2.22\\ 
     18 &  0.067  &   6.0   &    &             &  3.3& 2.22    & 7.8&  $>$10&     \\ 
     20 &  0.01  &    0.1   &    &             &     &         &0.13&       &     \\ 
     21 &  0.064  &   3.2   &    &             &  3.6& 1.61    & 4.1&  $>$11&     \\ 
     23 &  0.063  &   3.1   &    &             &  5.9& 0.89    & 4.0&  $>$18&     \\ 
     24 &  0.086  &   5.7   &    &             &  8.5& 1.89    & 7.4&  $>$26&     \\ 
     26 &  0.077  &   4.3   &    &             &  1.7& 1.28    & 5.6& $>$5.2&     \\ 
     31 &  0.063  &   2.6   &    &             &  1.9& 1.15    & 3.4& $>$5.8&     \\ 
     33 &  0.133  &  12.4   &    &             &     &         &16.1&       &     \\ 
     35 &  0.137  &  11.9   &    &             & 32.5& 5.30    &15.5&  $>$99&     \\ 
     38 &  0.107  &   6.9   &    &             &  6.7&         & 9.0&  $>$20&     \\ 
     39 &  0.269  &  47.6   &    &             &     & 2.23    & 62 &       &     \\ 
  40$^a$&  0.45   & 122.9   &    &             &     & 0.17    & 160&   2000&     \\ 
     41 &  0.12   &   8.6   &    &             &     & 1.22    &11.1&       &     \\ 
     43 &  0.21   &  27.5   &    &             & 21.1& 7.23    &  36&  $>$64&     \\ 
     49 &  0.127  &   9.8   &    &             &     & 3.39    &12.7&       &     \\ 
     \hline
\end{tabular}}
\medskip
$^a$ Data from  \citet{chapman02}, main component, reddening corrected H$\beta$ luminosity. 
\end{table}