\begin{table}%t1
\caption{ Source properties.}
%\centerline
{
%\scriptsize
\begin{tabular}{llcccccc}
\hline
\hline
\noalign{\smallskip}
Source &  Class  &   $z$  & $  N_{\rm H,Gal}$ & $ \log M_{\rm BH}^a $  &  $S_{\rm core,5GHz}^b$&  $S_{\rm tot,5GHz}^b$ &  $\Re^b$ \\    
\noalign{\smallskip}
       &         &      & $[{\rm 10^{20}~cm^{-2}}]$ &$[M_{\odot}]$ & [Jy]  & [Jy]     &  $[S_{\rm core}/S_{\rm ext}]$ \\     
\noalign{\smallskip}
\hline
\noalign{\smallskip}
\noalign{\smallskip}
  NGC~1692       & FRI &  0.035 &3.54 & 9.01 & 0.04 & 1.81 & 0.023 \\
\noalign{\smallskip}
\noalign{\smallskip}
 PKS~0625-35   & FRI &  0.055 &7.08 & 9.19 & 0.60 & 2.12 & 0.395 \\
\noalign{\smallskip}
\noalign{\smallskip}
3C~88        & FRI/FRII & 0.030  &8.81 & 8.70 & 0.16 & 2.14 & 0.087 \\
\noalign{\smallskip}
\noalign{\smallskip}
3C~444        & FRII& 0.153  &2.61 & 9.28 & $<$0.002& 1.99 & $<$0.0009\\
\hline
\end{tabular}}\medskip
 $^a$ From Bettoni et~al. (\cite{Bettoni2003}); the uncertainty is $\sim$0.4 dex.
$^b$ From Morganti et~al. (1993).
\label{tab1}
\end{table}