\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}