\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}