\begin{table}%t1
\par
\caption{\label{table1}Basic parameters of the observed sample.}
%\centerline
 {
\begin{tabular}{lllccrccrrrcl}
\hline \hline
\noalign{\smallskip}
Source & $z$  & Class & Ref. & $\log{\nu L^{{\rm total}}_{{\rm 408~MHz}}}$ & $\log{R}$ & Freq. & Ref. & $\frac{[\mbox{\ion{O}{iii}}]}{[\mbox{\ion{O}{ii}}]}$ & $\frac{[\mbox{\ion{O}{iii}}]}{[{\rm H}\beta]}$ & $\log{\nu L_{[\mbox{\scriptsize\ion{O}{iii}}]}}$ & Ref. & VISIR \\
&&&&&&&&&&&& Resolution \\
&&&&(erg s$^{-1}$)&&(GHz)&&&&(erg s$^{-1}$)&&(parsec) \\
(1)&(2)&(3)&(4)&(5)&(6)&(7)&(8)&(9)&(10)&(11)&(12)&(13) \\
\hline
4C12.03      & 0.15600 & LEG    & 5     & 41.98 & $ $ $-$2.66 &   1.5 &  5      &  $\dots$ &  $\dots$ & $ $ 40.9 & 7      & 1400 \\
3C~015        & 0.07300 & LEG    & 8     & 41.64 & $ $ $-$2.02 &   2.3 &  6      &  $\dots$ &  3.7     & $ $ 40.4 & 6      &  610 \\
3C~029        & 0.04503 & FR-I   & 8     & 41.26 & $ $ $-$1.79 &   2.3 &  6      &  $\dots$ &  1.7     & $ $ 39.9 & 6      &  370 \\
3C~040        & 0.01800 & FR-I   & 8     & 40.63 & $ $ $-$1.61 &   2.3 &  6      &  $\dots$ &  $\dots$ & $<$38.9 & 6      &  140 \\
3C~078        & 0.02865 & FR-I   & 8     & 40.94 & $ $ $-$0.92 &   2.3 &  6      &  $\dots$ &  $\dots$ & $<$39.1 & 6      &  230 \\
Fornax~A     & 0.00587 & FR-I   & 8     & 40.72 & $ $ $-$3.40 &   2.3 &  6      &  $\dots$ &  $\dots$ & $<$38.6 & 6      &   40 \\
3C~093        & 0.35700 & BLRG   & 6     & 43.02 & $ $ $-$2.38 &   5.0 &  2,7    &  3.9     &  $\dots$ & $\dots$  & 3      & 3500 \\
3C~098        & 0.03045 & HEG    & 5     & 41.31 & $ $ $-$2.70 &   8.3 &  4      &  2.9     & 15       & $ $ 40.9 & 1      &  240 \\
3C~105        & 0.08900 & HEG    & 8     & 41.80 & $ $ $-$2.27 &   2.3 &  6      &  $\dots$ & 16       & $ $ 40.8 & 6      &  750 \\
3C~120        & 0.03301 & BLRG   & 8     & 40.73 & $ $    1.01 &   2.3 &  6      &  5.7     &  $\dots$ & $ $ 41.8 & 6      &  270 \\
3C~135        & 0.12738 & HEG    & 5     & 42.05 & $ $ $-$2.71 &   8.3 &  3      &  $\dots$ &  $\dots$ & 42.0  & 9         & 1100 \\
Pictor~A     & 0.03506 & BLRG   & 8     & 42.22 & $ $ $-$1.57 &   2.3 &  6      &  1.8     &  4.2     & $ $ 41.2 & 6      &  280 \\
3C~198        & 0.08147 & HEG    & 3     & 41.56 & $ $ $-$2.20 &   5.0 &  1, 7    &  1.2     &  2.1     & $ $ 41.1 & 8      &  680 \\
3C~227        & 0.08583 & BLRG   & 8     & 42.13 & $ $ $-$2.55 &   2.3 &  6      & 13       &  9.0     & $ $ 41.8 & 6      &  710 \\
3C~270        & 0.00746 & FR-I   & 8     & 40.21 & $ $ $-$1.71 &   2.3 &  6      &  $\dots$ &  4.7     & $ $ 38.9 & 2,10   &   55 \\
Centaurus~A  & 0.00095 & FR-I   & 8     & 40.30 & $ $ $-$1.35 &   2.3 &  6      &  2.5     &  6.3     & $ $ 38.3 & 5, 6    &    7 \\
PKS1417$-$19 & 0.12000 & BLRG   & 4     & 41.79 & $ $ $-$2.20 &   5.0 &  7, 8    & 22       &  2.2     &  $\dots$ & 4      & 1000 \\
3C~317        & 0.03446 & FR-I   & 8     & 41.38 & $ $ $-$0.79 &   2.3 &  6      &  0.37    &  3.1     & $ $ 40.0 & 6      &  280 \\
3C~327        & 0.10480 & HEG    & 8     & 42.17 & $ $ $-$2.19 &   2.3 &  6      & 12       & 15       & $ $ 42.1 & 6      &  890 \\
3C~353        & 0.03042 & LEG    & 8     & 42.01 & $ $ $-$2.64 &   2.3 &  6      &  $\dots$ &  0.92    & $ $ 39.3 & 6      &  240 \\
PKS1839$-$48 & 0.11120 & LEG    & 8     & 41.99 & $ $ $-$1.16 &   2.3 &  6      &  $\dots$ &  $\dots$ & $<$39.2 & 6      &  960 \\
3C~403        & 0.05900 & HEG    & 8     & 41.59 & $ $ $-$2.18 &   2.3 &  6      &  8.4     & 20       & $ $ 41.6 & 6      &  490 \\
3C~403.1      & 0.05540 & LEG    & 7     & 41.04 &  $\dots$    &$\dots$&  $\dots$& $\dots$  &  $\dots$ & $\dots$  & $\dots$&  450 \\
3C~424        & 0.12699 & LEG    & 5     & 42.03 & $ $ $-$1.70 &   8.3 &  3      &  $\dots$ &  $\dots$ & $ $ 40.7 & 9      & 1100 \\
PKS2158$-$380& 0.03330 & HEG    & 2     & 40.56 & $<$ $-$1.92 &   5.0 &  7, 9    & $\dots$  &  $\dots$ &  $\dots$ & $\dots$&  270 \\
3C~445        & 0.05620 & BLRG   & 8     & 41.66 & $ $ $-$1.57 &   2.3 &  8      & 14       & 13       & $ $ 42.0 & 6      &  460 \\
PKS2354$-$35 & 0.04905 & FR-I   & 1     & 41.24 & $ $ $-$1.16 &   5.0 &  7, 10   & $\dots$  &  $\dots$ &  $\dots$ & $\dots$&  400 \\
\hline
\end{tabular}}
\par
\tablefoot {\textit{Column~(2)} Redshifts are from the NED catalogue, except for Centaurus~A, which is calculated from the distance from \cite{2004AetA...413..903R}. \textit{Column~(3)} Classifications: FR-I stands for Fanaroff-Riley class~I radio galaxy, LEG and HEG for low- and high-excitation Fanaroff-Riley class II radio galaxy and BLRG for broad-line radio galaxy. \textit{Column~(4)} References to classifications: 1~=~\cite{2006AJ....131..100B}, 2~=~\cite{1992ApJ...389..208B}, 3~=~\cite{1992MNRAS.256..186B}, 4~=~\cite{1978ApJ...220..783G}, 5~=~\cite{1998MNRAS.296..445H}, 6~=~\cite{1996AetA...313..423H}, 7~=~\cite{1997MNRAS.286..241J}, and 8~=~\cite{1997MNRAS.284..541M}. 
\textit{Column~(5)} Integrated radio source luminosities, at rest 408~MHz from \cite{1996yCat.8015....0W}. 
\textit{Columns~(6--8)} Radio core fraction, i.e. the ratio of the core to the extended radio flux at 1.5, 2.3, 5.0, or 8.0~GHz frequencies and references: 1~=~\cite{2003yCat.8071....0B}, 2~=~\cite{1994AetAS..105...91B}, 3~=~\cite{1998MNRAS.296..445H}, 4~=~\cite{1999MNRAS.304..135H}, 5~=~\cite{1991AJ....102..537L}, 6~=~\cite{1997MNRAS.284..541M}, 7~=~\cite{1996yCat.8015....0W}, 8~=~\cite{1995ApJ...448..521Z}, 9~=~\cite{1982MNRAS.201..991F}, and 10~=~\cite{1991ApJ...376..424S}.  \textit{Columns~(9--12)} Optical emission-line ratios of [\ion{O}{iii}] to [\ion{O}{ii}], [\ion{O}{iii}] to H$\beta$, and optical [\ion{O}{iii}] emission-line luminosities calculated from flux values found in the literature. References to emission-line ratios and fluxes: 1~=~\cite{1977ApJ...211..675C}, 2~=~\cite{1996ApJ...470..444F}, 3~=~\cite{2003ApJ...599..886E}, 4~=~\cite{1978ApJ...220..783G}, 5~=~\cite{2007ApJ...670L..81H}, 6~=~\cite{1993MNRAS.263..999T}, 7~=~\cite{2007AetA...470..531W}, 8~=~\cite{1996MNRAS.281..509S}, 9~=~\cite{2009AetA...495.1033B}, and 10~=~\cite{1997ApJS..112..315H}. \textit{Column~(13)} Scale of the VISIR mid-infrared diffraction-limit of $0.40\arcsec$ in parsecs.}
\vspace*{2mm}
\end{table}