\begin{table}%t7
\caption{Rate of radio-excess galaxies in the literature.}\label{tabla:exceso-rate}
\small %\centerline
{\begin{tabular}{lccccccccccc}
\hline \hline\noalign{\smallskip}
& &  \multicolumn{9}{c}{Rate of Radio-excess galaxies$^1$} & \\
\cline{3-11}
& & \multicolumn{3}{c}{Total} &\multicolumn{3}{c}{E-S0a} & \multicolumn{3}{c}{Sa-Irr} & \\
\cline{3-11}\noalign{\smallskip}
Sample & Environment & N$^2$ & F5$^3$ & F3$^3$ & N$^2$ & F5$^3$ & F3$^3$ & N$^2$ & F5$^3$ & F3$^3$ & Notes \\
\hline\noalign{\smallskip}
AMIGA$^4$ & Isolated & 397 & 0.8 & 4.0 & 21 & 4.7 & 19.1 & 376 & 0.5 & 2.1 &  $m_{B}<15$ \\
Condon (1991) &  --  &  122 &  32.0  &  33.6 & 11  &  90.9  &  90.9  &  71  &  9.9  & 12.7  & $S_{60~\mu{\rm m}} > 0.2~{\rm Jy}$ \\
& & &  & & &  &  & &  &  &  and $S_{4.85~{\rm GHz}} > 25~{\rm mJy}$ \\
Yun (2001) & -- & 1809 & 1.3 & -- & -- & -- & -- & -- & -- & -- & $S_{60~{\rm \mu m}}> 2~{\rm Jy}$\\
Corbett (2002) & -- & 82 & 2.4 & 4.9 & -- & -- & -- & -- & -- & -- & $S_{60~{\rm \mu m}}> 4~{\rm Jy}$\\
 Condon (2002)  & --  &  1897 & 8.2 &  10.8 &  287 & 42.2 & 51.6 & 1498 &  2.1 & 3.4 &
$S_{1.4~{\rm GHz}}>2.5~{\rm mJy}$ \\
&  & & &  & &  &  & &  &  & and $m_{\rm P}<14.5$ \\
 Drake (2003)  &  --  &  178  &   55.1  &  60.7   &  --  & -- &  --  &  --  &  --  &  -- & $S_{4.8~{\rm GHz}}\gtrsim 16~{\rm mJy}$ \\
 &  & &   & & & & &&  &  & and $S_{60~{\rm \mu m}} \gtrsim 0.1~{\rm Jy}$ \\
Omar (2005) & Eridanus group & 72 & 2.8 & 2.8 & 20 & 5.0 & 5.0 & 46 & 2.2 & 2.2 & \\
Niklas (1995) &  Virgo cluster & 37 & -- & 16.2 & 2 & -- & 0.0 & 35 & -- & 17.1 & radio@4.8~GHz \\
Andersen (1995) & Cluster \& group (poor) & 23 & 8.7 & 21.7 & -- & -- & -- & -- & -- & -- & \\
& Cluster \& group (rich) & 20 & 15.0 & 25.0 & -- & -- & -- & -- & -- & -- & \\
Miller (2001) & Clusters $0<r<1$~Mpc & 120 & 28.3 & 37.5 & 54 & 46.3 & 53.7 & 53 & 3.8 & 17.0 &
$S_{1.4~{\rm GHz}}>10~{\rm mJy}$ \\
 & Clusters $1<r<2$ Mpc & 96 & 21.9 & 29.2 & 23 & 60.9 & 73.9 & 50 & 6.0 & 10.0 & $S_{1.4~{\rm GHz}}>10~{\rm mJy}$ \\
 & Clusters $2<r<3$~Mpc & 94 & 6.4 & 12.8 & 19 & 26.3 & 31.6 & 47 & 0.0 & 4.3 & $S_{1.4~{\rm GHz}}>10~{\rm mJy}$ \\
Reddy (2004) & \mbox{X-ray} clusters & 114 & 13.2 & 19.3 & 33 & 30.3 & 45.5 & 81 & 6.2 & 8.6 & $L_{60~{\rm \mu m}}> 8.92~L_{\odot}$ \\
 & \mbox{X-ray} clusters core & 33 & 24.2 & 39.4 & 15 & 40.0 & 66.7 & 18 & 11.1 & 16.7 & $L_{60~{\rm \mu m}}> 8.92~L_{\odot}$ \\
 & \mbox{X-ray} clusters ring & 81 & 8.6 & 11.1 & 18 & 22.2 & 27.8 & 63 & 4.8 & 6.3 & $L_{60~{\rm \mu m}}> 8.92~L_{\odot}$ \\
\hline
\end{tabular}}
\medskip
$^{\rm 1}$ The percentages are computed over the number of galaxies for each morphological subsample;  $^{\rm 2}$ number of galaxies in the total samples or the morphological subsamples;
 $^{\rm 3}$ F3: factor~3 radio excess; F5: factor~5 radio excess. Figures given in percentages;
 $^{\rm 4}$ all percentages for the fraction of radio-excess galaxies are upper limits as explained in Sect.~\ref{sec:error}.
\end{table}