\begin{table}%t2
%\centering
\par
\caption{\label{tab:FFpart}Fractional fluxes at the locations of the WR stars\tablefootmark{a}$\!$.}
\begin{tabular}{lrrrr}
\hline\hline \noalign{\smallskip}
& ID\tablefootmark{b} & Subtype\tablefootmark{c}  &   Number & $FF$\tablefootmark{d}	\\
\hline
 &   1   &    WNL   & 	   3  &   0.29    \\  
  &  2   &    WCL   & 	   2  &   0.34    \\  
  &  3   &    WCL   & 	   2  &   0.26    \\  
{\bf M~83} &    4   &    WNE   & 	  16  &   0.48    \\ 
&    5   &    WCL   & 	   8  &   0.48    \\  
 &   6   &    WCE   & 	   3  &   0.06    \\  
&   ... &   ... &... & ...  \\ 
&  133   &    cand.   &   ...  &   0.25      \\  
&  134   &    cand.   &   ...  &   0.54      \\  
  \hline
&    1   &    WNE   & 	   1  &   0.37      \\  
 &   2   &    WCE   & 	   1  &   0.30      \\  
{\bf NGC~1313}&   3   &    WNL   & 	   1  &   0.06      \\
&    ... &  ... &... &  ...   \\ 
&   28   &    cand.   &  ...  &   0.38      \\  
\hline
\end{tabular} 
\tablefoot{\tablefoottext{a}{An indicative portion of this table is shown. For the full table refer  to the electronic version of the Journal.}
\tablefoottext{b}{We follow the exact numbering of \cite{M83} and \cite{NGC1313}. Additional info (e.g. fluxes, errors in star numbers) can be found in these references.} 
\tablefoottext{c}{``cand''.~stands for candidate region.}
\tablefoottext{d}{These fractional fluxes refer to a binning of 15 and 19 for the images of M~83 and NGC~1313 we have used, respectively. Although we have shown that the results do not change significantly with the choice of binning, individual fractional fluxes can vary.}}
\end{table}