\begin{table}%t1
%\centering
\par
  \caption{\label{wrdata}Detection of WR features and the nebular \ion{He}{ii} emission line for the galaxies analyzed in this work.}
\par
    \tiny
  \begin{tabular}{l@{\hspace{4pt}}c  c@{\hspace{8pt}}c c   c@{\hspace{8pt}}cc    c@{\hspace{8pt}}cc  c@{\hspace{8pt}}cc   }
    \hline\hline
\noalign{\smallskip}
 & & \multicolumn{2}{c@{\hspace{4pt}}}{\Hb} &  & 
\multicolumn{2}{c@{\hspace{4pt}}}{\HeII\ $\lambda$4686} & & 
\multicolumn{2}{c@{\hspace{4pt}}}{Blue\ \WRBUMP\tablefootmark{c}} & &
\multicolumn{2}{c@{\hspace{4pt}}}{Red\ \WRBUMP\tablefootmark{d}} & \\
\cline{3-4}
\cline{6-7}
\cline{9-10}
\cline{12-13}            
\noalign{\smallskip}
Galaxy & Zone &  
$I$  &  
$-W$   & 
$\eta$ &
$I$/$I$(\Hb) & 
$-W$ & &
$I$/$I$(\Hb) & 
$-W$ & &
$I$/$I$(\Hb) & 
$-W$ \\
 & & 
(a) & [\AA] & & 
(b) & [\AA] & &
(b) & [\AA] & &
(b) & [\AA] & \\
\noalign{\smallskip}    
\hline
\noalign{\smallskip}
 HCG 31& AC\tablefootmark{e}&46.13 $\pm$ 0.18 &  91.1 $\pm$ 2.1 & 0.25 & 0.9 $\pm$ 0.3 & 0.66 $\pm$ 0.22 &  & 3.2 $\pm$ 1.9 &  2.5 $\pm$ 0.6 & &  2.4 $\pm$ 0.6 & 3.1 $\pm$ 0.8 \\
                & F1    &  3.187 $\pm$ 0.016 &   218 $\pm$ 13  & 0.80 & 2.8 $\pm$ 0.3 & 4.3 $\pm$ 0.4 & & \nodata & \nodata & & \nodata & \nodata  \\
                & F2    &   2.28 $\pm$ 0.19  &   256 $\pm$ 43  & 0.80 & 2.2 $\pm$ 0.5 & 3.9 $\pm$ 1.5 & & 0.95 $\pm$ 0.35 & 3.4 $\pm$ 1.6  &&\nodata&\nodata\\
Mkn 1087        & C\tablefootmark{f} &   78.1           &  \nodata      & 0.25 & \nodata & \nodata & & 10.6 & \nodata & & \nodata & \nodata  \\
    Haro 15     &  C    &  23.3 $\pm$ 1.1    &  16.4 $\pm$ 1.1 & 0.40 & 0.49: & 0.08:  & & 2.82: & 0.5: & & \nodata &\nodata \\
                &  A    &  23.4 $\pm$ 0.9    &  75.7 $\pm$ 4.2 & 0.50 & 1.7 $\pm$ 0.4 & 1.0 $\pm$ 0.2 & & 1.4 $\pm$ 0.5 & 1.0 $\pm$ 0.3 & & \nodata&\nodata\\
    Mkn 1199    & C\tablefootmark{e} &  74.2 $\pm$ 3.1    &  21.4 $\pm$ 1.3 & 0.50 & 0.24: & 0.05:  & & 6.3 $\pm$ 1.8 & 1.3 $\pm$ 0.3 & & 9.4 $\pm$ 2.3 & 2.8 $\pm$ 0.7  \\
    Mkn 5       &  A    &  17.7 $\pm$ 0.7    &    75 $\pm$ 5   & 0.40 & 0.9 $\pm$ 0.2 & 1.6 $\pm$ 0.3 & & 1.5 $\pm$ 0.5 & 3.0 $\pm$ 1.2 & & \nodata &\nodata \\
IRAS 08208+2816 &  C    &  12.9 $\pm$ 0.5    &    80 $\pm$ 5   & 0.25 & \nodata & \nodata & & 4.1 $\pm$ 1.3 & 3.3 $\pm$ 1.0 & & 3.5 $\pm$ 1.3 & 3.6 $\pm$ 1.4 \\
IRAS 08339+6517 & \#1   &  36.5 $\pm$ 1.3    &    25 $\pm$ 2   & 0.50 & 0.48: & 0.1: & & 4.1: & 2.2: & & \nodata & \nodata  \\
POX 4 &  C    &  56.0 $\pm$ 1.8  & 200 $\pm$ 9   & 0.60 & 1.20 $\pm$ 0.16 & 1.9 $\pm$ 0.3 & & 1.5 $\pm$ 0.3 & 3.0 $\pm$ 0.9 & & 1.4 $\pm$ 0.2 & 3.9 $\pm$ 0.8  \\
         UM 420 &\nodata&  6.88 $\pm$ 0.27   &   169 $\pm$ 10  & 0.50 & 1.0 $\pm$ 0.2 & 2.0 $\pm$ 0.4 & & 1.5 $\pm$ 0.5 & 2.8 $\pm$ 0.7 & & \nodata&\nodata \\
SBS 0926+606    & A     &  16.2 $\pm$ 0.6    &   125 $\pm$ 6   & 0.60 & 0.7 $\pm$ 0.2 & 1.9 $\pm$ 0.3 & & 0.9:& 3.2: & & \nodata & \nodata \\
SBS 0948+532    &\nodata&  8.44 $\pm$ 0.32   &   213 $\pm$ 11  & 0.60 & 1.3 $\pm$ 0.3 & 1.6 $\pm$ 0.6 & & 1.1 $\pm$ 0.3 & 2.1 $\pm$ 0.7 & & \nodata & \nodata\\
SBS 1054+365    & C     &  14.6 $\pm$ 0.7    &    89 $\pm$ 7   & 0.40 & 0.6 $\pm$ 0.2 & 0.9 $\pm$ 0.3 & & 1.6 $\pm$ 0.5 & 2.4 $\pm$ 0.8 & & \nodata & \nodata\\
SBS 1211+540    &\nodata&  1.84 $\pm$ 0.09   &   135 $\pm$ 10  & 0.50 & \nodata & \nodata & & $<$1.2: & \nodata & & NO OBS.\tablefootmark{g}  & NO OBS.\tablefootmark{g}   \\
SBS 1319+579    & A     &  14.6 $\pm$ 0.5    &   285 $\pm$ 14  & 0.90 & 0.8: & 1.5: & & 0.7: & 1.9: & & \nodata & \nodata  \\
SBS 1415+437    & C     &  18.5 $\pm$ 0.7    &   222 $\pm$ 11  & 0.60 & 2.4 $\pm$ 0.2 & 4.8 $\pm$ 0.3 & & $<$0.9: & \nodata & & \nodata & \nodata \\
III Zw 107      & A     &  22.3 $\pm$ 0.8    &  44.2 $\pm$ 2.3 & 0.50 & \nodata & \nodata & & 3.1 $\pm$ 1.1 & 1.3 $\pm$ 0.4 & & \nodata & \nodata \\
Tol 9           & C     &  23.4 $\pm$ 0.9    &  33.3 $\pm$ 2.0 & 0.50 & 0.33 $\pm$ 0.15 & 0.24 $\pm$ 0.7 & & 7.9 $\pm$ 1.3 & 2.5 $\pm$ 0.4 & & 5.8: & 1.9: \\
Tol 1457-262    & A     &   222 $\pm$ 8      &   101 $\pm$ 6   & 0.50 & 1.9 $\pm$ 0.4 & 1.5 $\pm$ 0.3 & & \nodata & \nodata & & \nodata & \nodata \\
                & B     &  47.7 $\pm$ 2.3    &    83 $\pm$ 7   & 0.40 & 2.9 $\pm$ 0.3 & 2.1 $\pm$ 0.2 & & \nodata & \nodata & & \nodata & \nodata \\
ESO 566-7       &\nodata&  10.2 $\pm$ 0.8    &    13 $\pm$ 2   & 0.25 & \nodata & \nodata & & \nodata & \nodata & & \nodata & \nodata \\				
ESO 566-8       &\nodata& 111 $\pm$ 5  & 95 $\pm$ 7 & 0.50 & 0.74 $\pm$ 0.25 & 0.65 $\pm$ 0.25 & & 6.2 $\pm$ 2.2 & 4.1 $\pm$ 1.5 & & 4.8 $\pm$ 1.2 & 4.2 $\pm$ 1.2 \\
   NGC 5253     & A &  134.5 $\pm$ 0.4  &  234 $\pm$ 5   & 1.00 & 0.10 $\pm$ 0.04 & 0.21 $\pm$ 0.09 & & 0.71 $\pm$ 0.12 & 1.6 $\pm$ 0.3 & & NO OBS.\tablefootmark{g} & NO OBS.\tablefootmark{g} \\
                & B &  135.2 $\pm$ 4.2  &  254 $\pm$ 5   & 1.10 & 0.05: & 0.11: & & 0.71 $\pm$ 0.13 & 1.7 $\pm$ 0.3 & & NO OBS.\tablefootmark{g} & NO OBS.\tablefootmark{g}  \\
   %            & C\tablefootmark{e},\tablefootmark{g} &  101.3 $\pm$ 3.3  & 94.0 $\pm$ 1.0 & 0.40 & 0.06: & 0.05: & & 4.45 $\pm$ 0.21 & 3.82 $\pm$ 0.19 & & NO OBS. & NO OBS. \\
                & C\tablefootmark{e},\tablefootmark{g} &  101.3 $\pm$ 3.3  & 94.0 $\pm$ 1.0 & 0.40 & 0.06: & 0.05: & & 4.13 $\pm$ 0.19 & 3.55 $\pm$ 0.17 & &1.00 $\pm$ 0.14\tablefootmark{h}&NO OBS.\tablefootmark{g}\\
                & D &  25.6 $\pm$ 0.9   & 39.0 $\pm$ 0.5 & 0.30 & 0.40 $\pm$ 0.11 &  0.12 $\pm$ 0.04 & & \nodata & \nodata & & NO OBS.\tablefootmark{g} & NO OBS.\tablefootmark{g}\\	   
	\noalign{\smallskip}    
  \tableline
  \end{tabular}
   \tablefoot{\tablefoottext{a}{In units of 10$^{-15}$ erg s$^{-1}$ cm$^{-2}$ and not corrected for extinction.}
 \tablefoottext{b}{Assuming $I$(\Hb) = 100 and reddening-corrected.}
 \tablefoottext{c}{Broad \ion{He}{ii} $\lambda$4686 emission line only.}
  \tablefoottext{d}{Broad \ion{C}{iv} $\lambda$5808 emission line only.}
  \tablefoottext{e}{Broad \ion{N}{iii} $\lambda$4640 also detected. The reddened-corrected $I$/$I$(\Hb) ratios are 0.91, 5.6 and 1.44 for HCG~31~AC, Mkn~1199 and NGC~5253~C, respectively. See text for details.}
  \tablefoottext{f}{Data from \citet{Va97}, see \citet{LSER04b}. }
  \tablefoottext{g}{NO OBS indicates that the spectral range where the feature lies was not observed.}
  \tablefoottext{h}{ Broad \ion{C}{iv} $\lambda$4658 detected. The $I$/$I$(\Hb) ratio given here is assuming $L_{\rm WCE}$($\lambda$5808) = $L_{\rm WCE}$($\lambda$4658)/1.71 (SV98). See text for details.}}\vspace*{1.5mm}
\end{table}