\begin{table}%t2
        \caption{\label{tabv}Results of kinematical analysis.}
                $$
         \begin{array}{l r l l}
            \hline
                        \hline
            \noalign{\smallskip}
{\rm Sample} & N_{\rm g} & \phantom{249} {\langle v\rangle}\phantom{249} & 
\phantom{24}\sigma_{v}^{{a}}\phantom{24}\\
& &\phantom{249}{\rm km\ s^{-1}}\phantom{249} 
&\phantom{2}{\rm km\ s^{-1}}\phantom{24}\\
            \hline
            \noalign{\smallskip}
 {\rm Whole\ system\ (sample\ A)} & 68 &84~505\pm163 &1334_{-95}^{+114}\\ \noalign{\smallskip}
{\rm Blue\ galaxies }         & 11 &85~954\pm487 &1509_{-507}^{+763}\\ \noalign{\smallskip}
{\rm Red\ galaxies }          & 56 &84~288\pm167 &1243_{-85}^{+120}\\ \noalign{\smallskip}
{\rm Whole\ system\ (sample\  B)} & 69 &84~790\pm163 &1349_{-63}^{+112}\\ \noalign{\smallskip}
{\rm Sample\ A\ without\ KMM4g3\ gals} & 61 &84~296\pm174 &1353_{-97}^{+122}\\
              \noalign{\smallskip}
            \hline
         \end{array}
$$
\begin{list}{}{}  
\item[$^{{a}}$] We use the biweight and the gapper estimators by
Beers et al. (1990) for samples with $N_{\rm g}\ge 15$ and with
$N_{\rm g}<15$ galaxies, respectively (see also Girardi et
al. \cite{gir93}).
\end{list}
         \end{table}