\begin{table}%T6
\par
%\centering
\par
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\caption{The radio power of our sample for continuous emission and flares. The radio detections in M~82 are probably SNRs while in NGC~4736 we probably detect the nucleus of the galaxy. For all other sources we present upper limits for continuous emission over all epochs and flares. The distances are taken from \protect\citet{Tully1988}.}
\label{tableRadPower}
\begin{tabular}{llllc}
\hline \hline
Name & Dist. & $L_{\rm X}$ & $L_{\rm R,flare}$ & $L_{\rm R,cont}$\\
 & [Mpc] & $[ 10^{39}~ {\mbox{erg}~{\rm s}^{-1}}] $ & $[ 10^{33} ~{\mbox{erg}~{\rm s}^{-1}}] $
 & $[ 10^{33}~{\mbox{erg}~{\rm s}^{-1}}] $ \\
\hline
M~33 & 0.7 & 1 & $< $0.43  & $< $0.2 \\     
NGC~2403 & 4.2 & $2$ & $<$13 & $<$5.4 \\
M~82-D & 5.2 & $3$ & $< $45 & 290 \\
M~82-F & 5.2 &$6$ & $< $45 & 307 \\
NGC~4736-1 &4.3 &$1$ & $< $21 & 177 \\
NGC~4736-2 & 4.3 & $1$ & $< $21 & $< $9.2  \\ 
NGC~5204 & 4.8& $2$ & $< $18  & $< $7.1 \\ 
NGC~5457-1 &5.4& $2$ & $< $23 & $< $9.1 \\
NGC~5457-2 &5.4& $1$ & $< $23 & $< $9.1 \\
\hline
\end{tabular}
\end{table}