\begin{table}%t5
%\centering
\par
\caption{\label{tab_wr_flux}Properties of WR~stars in GRB hosts.}
\par
\begin{tabular}{ccccccccccc}
\hline \hline\noalign{\smallskip}
\rm{Ion} & \multicolumn{2}{c}{980703} & \multicolumn{2}{c}{020405} &
\multicolumn{2}{c}{020903} & \multicolumn{2}{c}{031203} &
\multicolumn{2}{c}{060218} \\
\hline
& $F$ & $L$ &   $F$ & $L$ &  $F$ & $L$ &  $F$ & $L$ &  $F$ & $L$ \\
\hline
$\rm{blue\ bump}$ ($\lambda4650$)\tablefootmark{a} & -- & -- & $0.18 \pm 0.09$ & $654.39 \pm 326.21$ & $1.52 \pm 0.31$ & $97.22 \pm 42.90$ & $10.65 \pm 6.06$ & $114.87 \pm 65.37$ & $8.08 \pm 3.25$ & $6.49 \pm 2.41$ \\
$\rm{red \ bump}\ (\lambda$5008) & -- & -- & -- & -- & $0.50\pm0.10$ & $32.10 \pm 7.30$ & -- & -- & -- & -- \\
\rm{CIII}$\lambda5696$ & -- & -- & -- & -- & -- & -- & -- & -- & 3.76~$\pm$~1.10 & $2.48\pm0.76$ \\
\hline
WNL &
\multicolumn{2}{c}{--} & \multicolumn{2}{c}{--} &
\multicolumn{2}{c}{$2117 \pm 721$} & \multicolumn{2}{c}{5743~$\pm$~3268} &
\multicolumn{2}{c}{$324 \pm 120$} \\ 
WCE & \multicolumn{2}{c}{--} & \multicolumn{2}{c}{--} & \multicolumn{2}{c}{$1070 \pm 210$} &
\multicolumn{2}{c}{--} & \multicolumn{2}{c}{--} \\
WCL & \multicolumn{2}{c}{--} & \multicolumn{2}{c}{--} &
\multicolumn{2}{c}{--} & \multicolumn{2}{c}{--} &
\multicolumn{2}{c}{$31 \pm 10$} \\ 
WR/O & \multicolumn{2}{c}{--} & \multicolumn{2}{c}{$0.04\pm0.03$} &
\multicolumn{2}{c}{$0.21 \pm 0.06$} & \multicolumn{2}{c}{$0.01 \pm 0.01$} &
\multicolumn{2}{c}{$0.11 \pm 0.04$} \\
\hline
\end{tabular}
\tablefoot{WR emission line fluxes ($F$, corrected for Galactic extinction) are in units of $10^{-17}~\rm{erg}~\rm{s}^{-1}~cm^{-2}$, Luminosities ($L$) are in units of $10^{38}~\rm{erg}~\rm{s}^{-1}$. 
\tablefoottext{a}{Fluxes and luminosities of nebular lines were subtracted.}}
\end{table}