\begin{table}%t3
\caption{Radio-excess ratios for the complete subsample$^1$.}\label{tabla:exceso}
\small %\centerline
 {\begin{tabular}{ccccccccc}
\hline \hline\noalign{\smallskip}
\multirow{3}{*}{Morpho$^3$} & \multicolumn{4}{c}{Radio-excess galaxies} & \multicolumn{4}{c}{FIRST revised$^2$} \\
\cline{2-9}
 & \multicolumn{2}{c}{Factor~5} & \multicolumn{2}{c}{Factor~3} & \multicolumn{2}{c}{Factor 5} & \multicolumn{2}{c}{Factor~3} \\
\cline{2-9}
 & N & \% & N & \% & N & \% & N & \% \\
\hline
All T ($n=397$) & 6 & 1.5 & 16 & 4.0 & 3 & 0.8 & 12 & 3.0 \\
E-S0a ($n=21$)  & 1 & 4.8 & 4  & 19.1 & 1 & 4.8 & 4  & 19.1 \\
Sa-Irr ($n=376$) & 5 & 1.3 & 12 & 3.2 & 2 & 0.5 & 8  & 2.1 \\
\hline
\end{tabular}}
\medskip
$^{\rm 1}$ All percentages for the fraction of radio-excess galaxies are upper limits as explained in Sect.~\ref{sec:error}. 
  $^{\rm 2}$  In Sect.~\ref{sec:error} we explain how we revise these numbers using the FIRST survey.  $^{\rm 3}$  Morphological subsamples. The percentages are computed over the number of galaxies for each subsample.
\end{table}