\begin{table}%T4
\caption{\label{t:WR_broad}Parameters of the WR lines and of the broad components.}
%%\centerline
\par
{
\begin{tabular}{lrr} \hline \hline
\rule{0pt}{10pt}
& MMT & BTA    \\ \hline
\MC{3}{c}{Flux (10$^{-16}$ ergs\ s$^{-1}$cm$^{-2}$)$^a$}    \\
4640\ N\  {\sc iii}\ (WR)\  &   2.5 &   3.8 \\
4658\ C\  {\sc iv}\ (WR)\   &   2.6 &   5.0 \\
4686\ He\ {\sc ii}\  (WR)\  &   2.4 &   3.7 \\
4861\ H$\beta$\             &   6.3 &  15.0 \\
4959\ [O\ {\sc iii}]\       &  11.6 &  18.3 \\
5007\ [O\ {\sc iii}]\       &  34.8 &  55.0 \\
6563\ H$\alpha$\            & 159.4 & 261.3 \\  \hline
\MC{3}{c}{Equivalent width [\AA]}                         \\
4640\ N\  {\sc iii}\ (WR)\  &   1.4 &   2.1 \\
4658\ C\  {\sc iv}\ (WR)\   &   1.5 &   2.8 \\
4686\ He\ {\sc ii}\  (WR)\  &   1.4 &   2.1 \\
4861\ H$\beta$\             &   4.0 &   7.8 \\
4959\ [O\ {\sc iii}]\       &   7.9 &   9.8 \\
5007\ [O\ {\sc iii}]\       &  24.3 &  30.0 \\
6563\ H$\alpha$\            & 238.4 & 302.2 \\  \hline
\MC{3}{c}{{\it FWHM} [km s$^{-1}$]}                         \\
4640\ N\  {\sc iii}\ (WR)\  & 1300 &  1300 \\
4658\ C\  {\sc iv}\ (WR)\   & 1300 &  1300 \\
4686\ He\ {\sc ii}\  (WR)\  & 1300 &  1300 \\
4861\ H$\beta$\             & 1500 &  1500 \\
4959\ [O\ {\sc iii}]\       & 1500 &  1500 \\
5007\ [O\ {\sc iii}]\       & 1500 &  1500 \\
6563\ H$\alpha$\            & 1300 &   900 \\  \hline
\MC{3}{c}{Broad/Nebular flux ratio [\%]}               \\
4686\ He\ {\sc ii}\  (WR)\  & 36  &  46 \\
4861\ H$\beta$\             & 1.9 & 3.5  \\
4959\ [O\ {\sc iii}]\       & 1.7 & 2.2  \\
5007\ [O\ {\sc iii}]\       & 1.7 & 2.2  \\
6563\ H$\alpha$\            & 16  &  22 \\  \hline
\MC{3}{c}{WR/O stars ratio}                      \\
Observed                    & \MC{2}{c}{0.02~~~~~~~~~~~~~~~~~~~~}  \\
Model$^b$                   & \MC{2}{c}{0.02~~~~~~~~~~~~~~~~~~~~} \\
\hline \end{tabular}}
\smallskip
$^a$ Flux errors are~$\sim$50\% for the broad \ion{He}{ii}~$\lambda$4686 line. 
and~$\sim$(15--25)\% for the broad components of the strong lines.\\
$^b$ Data from Schaerer \& Vacca (\cite{SV98}).\\
\end{table}