\begin{table}%T7
\caption{\label{tab_wrmodif}Some spectral properties derived from the observed stellar content
(2nd~column) and from the one with BSG, WR and whole population replaced with
the one predicted by the fitted power-law IMF (3rd, 4th and~5th~columns,
respectively).~$Q(X)$ designates the photon rate able to ionize the ion "X''
population of a nebula.~$^a$The 5th and 6th~columns correspond to analytical
models, whose total mass here reproduce the observed {\it F439W}~luminosity.
$^b$Best-fit model of the canonical analysis.}
%\centering
\par
\begin{tabular}{lccccc}
\hline\hline
BSG content & Real & IMF & Real & IMF$^a$ & 2.8 Myr$^{a,b}$ \\
WR content &  Real & Real & IMF & IMF$^a$ & 2.8 Myr$^{a,b}$ \\
MS content &  Real & Real & Real & IMF$^a$ & 2.8 Myr$^{a,b}$ \\
\hline
$W({\rm H}\beta)$ ({\AA})& 342 & 133 & 284 & 80 & 247 \\
$Q({\rm H}^0)$ ($10^{50}$ s$^{-1}$)& 2.14 & 2.16 & 1.39 & 0.54 & 1.60 \\
$Q({\rm He}^0)/Q({\rm H}^0)$& 0.13 & 0.12 & 0.14 & 0.11 & 0.14 \\
$10^8$~$Q({\rm He}^+)/Q({\rm H}^0)$& 9.3 & 8.0 & 2.8 $\times$ 10$^4$ & 8.8 & 130\\
$Q({\rm O}^+)/Q({\rm H}^0)$& 0.020 & 0.020 & 0.024 & 0.011 & 0.017 \\
\hline
\end{tabular}
\end{table}