\begin{table}%t1
  \caption{The sample. 
    $P_{\rm 178}$ in Col.~(3) is total radio power (W~Hz$^{-1}$sr~$^{-1}$) 
    at rest-frame 178~MHz. Column~(4) lists spectral index between 178 and 
    750~MHz, and Cols.~(5) and~(6) the radio morphology and emission-line type. 
    Apparent magnitude in rest-frame $R_{\rm C}$-filter and corresponding
    references are listed in Cols.~(7) and~(8). Columns~(9) and~(10) show
    velocity dispersion measurements from the literature (km~s$^{-1}$) 
    and corresponding references. The last three~columns list emission line 
    fluxes in units of 
    10$^{-15}$~erg~s$^{-1}$~cm$^{-2}$, both from the literature
    and as determined from our wide slit spectrophotometry, and references.}\label{table:t1}
\small%\centerline
{
\begin{tabular}{lllllllllllll}
\hline\hline
Radio ID  & Redshift & $\log P_{178}$& $\alpha_{178}^{750}$ 
    &\multicolumn{2}{c}{ } & $m_{R_{\rm C}}$ &  Ref. & $\sigma_{\rm lit}$ & Ref. & $S_{\rm [OII]}$ & $S_{\rm [OIII]}$ & Ref. \\
   (1)     &  (2)      &     (3)      &  (4) & (5) &  (6)  &  (7) & (8) & (9) & (10) & (11) & (12) & (13) \\
\hline
3C 20    &   0.174  & 26.49 & 0.66 & FRII & HEG & 16.80 & 1 & & & 0.634 & 1.915 & W \\
3C 28    &  0.1971 & 26.22 & 1.06 & FRII & LEG & 18.34 &  2 & & & 5.956 & ... & W \\
3C 31    &  0.0167 & 23.99 & 0.57 & FRI  & LEG & 11.92 & 2 & 249 & SHI90 & ... & 10.349 & G \\
3C 33    &  0.0595 & 25.60 & 0.76 & FRII & HEG & 14.80 & 3 & & & 33.017 & 147.48 & W \\
3C 35    &  0.0673 & 24.99 & 0.77 & FRII & LEG & 14.94 & 1 & & & 1.0 $\pm$ 0.2 & $<$0.34 & A \\
3C 66B   &  0.0215 & 24.35 & 0.50 & FRI & LEG & 12.55 & 2 & & & 6.782 & 4.801 & W \\
3C 76.1  &  0.0324 & 24.41 & 0.77 & FRI & LEG & 14.06 & 2 & 246 & SHI90 & $<$3.0 & $<$2.0 & A \\
3C 83.1B &  0.0255 & 24.53 & 0.62 & FRI & LEG & $<$12.11  & 4 & & & & & \\
3C 98    &  0.0306 & 24.95 & 0.78 & FRII & HEG & 14.18 & 3 & 175 & SHI90 & 7.936 & 39.775 & W \\
3C 381   &  0.1605 & 26.01 & 0.81 & FRII & HEG & 18.05 & 5 & & & 1.177 & 44.31 & W \\
3C 386   &  0.0170 & 24.13 & 0.59 & FRI & LEG & $<$12.21 & 4 & & & & & \\
3C 388   &  0.0908 & 25.64 & 0.70 & FRII & LEG & 14.12 & 3 & 365 & H85 & 1.618 & 1.901 & W \\ 
3C 401   & 0.201  & 26.32 & 0.71 & FRII & LEG & 16.68 & 6 & & & ... & 1.192 & W \\
3C 433   & 0.1016 & 26.10 & 0.75 & FRII & HEG & 16.59 & 5 & & & ... & 2.656 & W \\
3C 442A  & 0.0263 & 24.35 & 0.96 & FRII & LEG & 14.07 & 2 & 197 & SHI90 & 8.0 $\pm$ 0.8 & 4.7 $\pm$ 1.0 & A \\
3C 449   &  0.0171 & 23.82 & 0.58 & FRI  & LEG & 13.05 & 2 & 222 & SHI90 & $<$3.0 & $<$2.0 & A \\
3C 452   & 0.0811 & 25.88 & 0.78 & FRII & HEG & 17.16 & 7 & & & 17.149 & ... & W\\
3C 465   & 0.0305 & 24.87 & 0.75 & FRI  &  LEG & 13.14 & 2 & 341 & FIF95 & 2.0 $\pm$ 0.4 & $<$4.0 & A \\
4C 11.71 & 0.0262  & 24.12 & 0.75 & FRI  & LEG & 14.00 & 7 & 249 & EFAR99 & $<$5.0 & $<$3.0 & A \\
4C 12.03 & 0.157  & 25.77 & 0.87 & FRII & LEG & 15.91 & 1 & & & ... & 1.394 & W \\
4C 35.40 &  0.0301 & 24.29 & 0.76 & FRI  & LEG & 12.83 &  8$^{{\rm }}$ & 204 & EFAR99 & 1.0 $\pm$ 0.2 & $<$1.3 & A \\
\hline
\end{tabular}}
\medskip
References for $m_{R_{\rm C}}$: (1) Converted from
  $K_{\rm UKIRT}$ \citep{ll84} assuming $R_{\rm C}-K=2.5$
  \citep{dunlop03}; (2) \cite{cr04}; (3) \cite{ol89}; (4)
  \cite{martel99} (upper limit given because of contamination by
  foreground star); (5) converted from $V$ \citep{sh89} assuming
  $V-R_{\rm C}=0.61$ \citep{fukugita95}; (6) converted from $K$
  \citep{lebofsky81} assuming $R_{\rm C}-K$=2.5 \citep{dunlop03}; (7)
  converted from $V$ \citep{sandage73} assuming $V-R_{\rm C}=0.61$
  \citep{fukugita95}; (8) converted from 2MASS $K_{\rm s}$ assuming
  $R-K_{\rm s}=2.5$ \citep{dunlop03}. Emission-line classifications are
  from \cite{jr97}, except for 3C~28 and 4C~12.03 which are from
  Willott's compilation ({\tt
    http://www-astro.physics.ox.ac.uk/{$\sim$}{cjw}/3crr/3crr.html}), and
  3C~442A which we classify as LEG based on our Palomar spectrum.  The
  1.4~GHz fluxes were taken from NVSS by \cite{condon98} and from the
  surveys of \cite{wb92} and \cite{lp80}.  References for velocity
  dispersions: SHI90: \citet{smith90}, H85: \citet{heckman85}, FIF95:
  \citet{fif95} and EFAR99: \citet{efar99}.  References for
  emission-line fluxes: A: from our data, W and G: from Willott's and
  Grimes' compilations, respectively ({\tt
    http://www-astro.physics.ox.ac.uk/$\sim$cjw/3crr/3crr.html} and {\tt
    http://www-astro.physics.ox.ac.uk/$\sim$sr/grimes.html}).
\end{table}