\begin{table}%t1 %\centering \par \caption{\label{tab:galprop}Key properties of M~83 and NGC~1313\tablefootmark{a}.} \begin{tabular}{lcccccccccccc} \hline\hline \noalign{\smallskip} Galaxy & Metallicity & $D$ & Pix. scale\tablefootmark{b} &$M_B$ &$M_K$& Morph. & Conf. reg.\tablefootmark{c} &WN\tablefootmark{d} & WC\tablefootmark{d} &Cand. reg.\tablefootmark{e}\\ &\tiny{($\log$(O/H)+12)} &(Mpc) &(pc$^2$~pix$^{-1}$) & (mag) & (mag) & & &WNE$+$WNL & WCE$+$WCL & \\ \hline M~83 & 9.0 & 4.5 & 5.3$^2$ & $-$20.2 & $-$23.7 & SAB(s)c & 132 & 232$+$250 & 28$+$526 & 89 \\ NGC~1313 & 8.23 & 4.1 & 4.0$^2$ & $-$18.9 & $-$20.1 & SB(s)d & 70 & 29$+$22 & 34$+$0 & 12$^f$ \\ \hline \end{tabular} \tablefoot{\tablefoottext{a}{Compiled from \cite{M83,NGC1313} and NED.} \tablefoottext{b}{In the images from ESO/MPI 2.2~m (+WFI) and VLT/FORS used in the analysis. A galaxy at $z=0.01$ in the SDSS 2.5~m images used by K08 would have $\sim$80$^2$ pc$^2$ pix$^{-1}$.} \tablefoottext{c}{Confirmed regions containing one or more WR stars.} \tablefoottext{d}{Total number of stars per subtype used in this paper. These numbers may differ slightly from those reported in the literature, for the following reasons: WN5-6 stars have been included in the WNE distribution; WO in WCE; transitional WN/WC have been included in both WN and WC. The total number of WR stars is obtained by adding their corresponding subtypes.} \tablefoottext{e}{Candidate regions for which spectroscopy has not been conducted.} \tablefoottext{f}{11 of these are photometrically consistent with WN stars.}} \end{table}