\begin{table}%t4
  \caption{Dereddened line intensity ratios with respect to $I$(H$\beta$)~$=$ 100 for the three brightest star-forming bursts observed in Mkn~1087: the center of Mkn~1087~(C), the north companion galaxy~(N) and the intense burst~\#7. All have been observed both with 4.2~m WHT and 2.5~m~INT. Correction for underlying stellar absorption in \ion{H}{i}~Balmer lines has been also applied.}
  \label{table4a}  
%\centerline
{
  \begin{tabular}{lrcccccc}
    \hline\hline
	Line  & $f$($\lambda$)  &   C WHT      &   C INT      &  N  WHT    &   N  INT     &  \#7 WHT    &  \#7 INT     \\
	\hline    
 3726 $[$O II$]$  & 0.27  &206 $\pm$ 11$^a$&226 $\pm$ 13$^a$&155 $\pm$ 12  &325 $\pm$ 26$^a$&85.5 $\pm$ 7.1 &212 $\pm$ 20$^a$\\
 3729 $[$O II$]$  & 0.27  & \nodata      & \nodata      &231 $\pm$ 14  &  \nodata     &106 $\pm$ 8    &  \nodata     \\
 3869 $[$Ne III$]$& 0.23  &8.3 $\pm$ 2.9   &8.7 $\pm$ 3.3   &43.4 $\pm$ 6.9&37.8 $\pm$ 9.1  &9.9 $\pm$ 3.6  &17.1 $\pm$ 6.2  \\ 
 3889 He I+H8	  & 0.22  &13.8 $\pm$ 4.3  &7.6 $\pm$ 2.6   &\nodata     &\nodata       &15.0 $\pm$ 4.3 &15.6 $\pm$ 4.6  \\
 3968 $[$Ne III$]$& 0.21  &9.7 $\pm$ 3.5   &3.54:         &\nodata     &\nodata       &11.0 $\pm$ 3.6 &13.2 $\pm$ 3.7  \\
 4068 $[$S II$]$  & 0.19  &2.23:         &\nodata       &\nodata     &\nodata       &\nodata      &\nodata       \\
 4076 $[$S II$]$  & 0.19  &1.13:         &\nodata       &\nodata     &\nodata       &\nodata      &\nodata       \\
 4101 H$\delta$  & 0.18   &25.9 $\pm$ 4.3  &25.9 $\pm$ 4.6  &25.9 $\pm$ 4.8&25.9 $\pm$ 7.7  &25.9 $\pm$ 4.4 &25.9 $\pm$ 4.7  \\ 
 4340 H$\gamma$  & 0.135  &46.9 $\pm$ 4.7  &46.9 $\pm$ 5.2  &46.9 $\pm$ 7.2&46.9 $\pm$ 8.8  &46.9 $\pm$ 8.1 &46.9 $\pm$ 9.8  \\
 4363 $[$O III$]$ & 0.13  &1.76:         &\nodata       &\nodata     &\nodata       & \nodata     &1.85:         \\
 4471 He I	     & 0.10   &2.14:         &3.90 $\pm$ 1.5  &\nodata     &\nodata       &3.23:        &\nodata       \\
 4861 H$\beta$   & 0.00   &100 $\pm$ 5     &100 $\pm$ 6     &100 $\pm$ 5   &100 $\pm$ 7     &100 $\pm$ 5    &100 $\pm$ 6     \\
 4959 $[$O III$]$&$-$0.02 &32.2 $\pm$ 2.3  &33.9 $\pm$ 2.7  &78.2 $\pm$ 5.4&124 $\pm$ 7     &69.0 $\pm$ 5.5 &57.7 $\pm$ 6.1  \\
 5007 $[$O III$]$&$-$0.03 &97.4 $\pm$ 5.9  &109 $\pm$ 7     &218 $\pm$ 10  &375 $\pm$ 19    &201 $\pm$ 12   &161 $\pm$ 10    \\
 5016 He I	    &$-$0.03  &1.18:         &\nodata       &\nodata     &\nodata       &\nodata      &\nodata       \\
 5200 $[$N I$]$  &$-$0.05 &\nodata       &2.97 $\pm$ 0.79 &\nodata     &\nodata       &\nodata      &\nodata       \\
 5518 $[$Cl III$]$&$-$0.17&\nodata       &0.94:         &\nodata     &\nodata       &\nodata      &\nodata       \\
 5876 He I	    &$-$0.23  &10.3 $\pm$ 1.2  &11.1 $\pm$ 1.9  &12.6 $\pm$ 2.2&14.5 $\pm$ 2.4  &10.3 $\pm$ 1.3 &12.6 $\pm$ 1.9  \\
 6300 $[$O I$]$  &$-$0.30 &6.73 $\pm$ 0.60 &7.56 $\pm$ 0.76 &19.1 $\pm$ 3.0&9.7 $\pm$ 2.2   &4.55 $\pm$ 0.79&4.9 $\pm$ 1.9   \\
 6364 $[$O I$]$  &$-$0.31 &1.83:         &1.77:         &\nodata     &\nodata       &1.41:        &\nodata       \\
 6548 $[$N II$]$ &$-$0.34 &31.4 $\pm$ 2.7  &31.5 $\pm$ 3.3  &8.0 $\pm$ 1.7 &9.4 $\pm$ 3.3   &14.2 $\pm$ 1.9 &14.9 $\pm$ 2.2  \\ 
 6563 H$\alpha$ &$-$0.34  &286 $\pm$ 11    &286 $\pm$ 12    &286 $\pm$ 12  &286 $\pm$ 14    &286 $\pm$ 12   &286 $\pm$ 14    \\
 6584 $[$N II$]$ &$-$0.34 &102.2 $\pm$ 6.4 &98.1 $\pm$ 8.8  &22.6 $\pm$ 2.7&22.8 $\pm$ 4.1  &43.1 $\pm$ 3.0 &46.5 $\pm$ 5.4  \\ 
 6678 He I	    &$-$0.35  &1.84:         &\nodata       &\nodata     &10.3 $\pm$ 2.9  &2.09:        &\nodata       \\
 6716 $[$S II$]$ &$-$0.36 &42.9 $\pm$ 3.8  &43.8 $\pm$ 3.9  &48.7 $\pm$ 4.9&34.8 $\pm$ 4.3  &31.0 $\pm$ 3.4 &32.0 $\pm$ 5.7  \\
 6731 $[$S II$]$ &$-$0.36 &36.0 $\pm$ 2.9  &35.1 $\pm$ 4.2  &37.4 $\pm$ 4.1&27.4 $\pm$ 3.6  &23.7 $\pm$ 2.2 &26.4 $\pm$ 2.9  \\
\hline
\end{tabular}}
\medskip
   $^a$ $[$O II$]$ $\lambda\lambda$3726,3729 emission flux.
\end{table}