\begin{table}%t2
        \caption{Results of the kinematical analysis.}
         \label{tabv}
  $$
         \begin{array}{l r l l c}
            \hline
                       \hline
   {\rm Sample} & N_{\rm g} & \phantom{249}{\langle v\rangle}\phantom{249} & 
\phantom{24}\sigma_{v}^{{a}}\phantom{24}& {\rm BCM\ 
galaxies}\\
& &\phantom{249}{\rm km\ s^{-1}}\phantom{249} 
&\phantom{2}{\rm km\ s^{-1}}\phantom{24} & \\
            \hline
            \noalign{\smallskip}
\par
{\rm Whole\ system}         &85 &57817\pm148 &1362_{-108}^{+126}& 
{\rm A,B,C,D}\\
{\rm Whole\ system\ Sample2}&80 &57956\pm132 
&1175_{-76}^{+95}&{\rm A,B,C}\\[0.5mm]
{\rm WGAP1}        & 8 &54448\pm212 & 529_{-44}^{+124}&{\rm D}\\[0.5mm]
{\rm WGAP2}        & 6 &55912\pm78  & 162_{-55}^{+39}& \\[0.5mm]
{\rm DS-A}         &11 &59199\pm263 & 
816_{-103}^{+128}&{\rm A}\\[0.5mm]
{\rm DS-C}          & 3 &56138\pm1001& - &{\rm C}  \\[0.5mm]
{\rm KMM1}         &10 &54819\pm299 & 873_{-114}^{+225}&{\rm D} \\[0.5mm]
{\rm KMM2}      &44 &57833\pm155 &1017_{-77}^{+109}&{\rm B,C} \\[0.5mm]
{\rm KMM3}      &31 &58500\pm203 &1109_{-112}^{+199}&{\rm A} \\[0.5mm]
{\rm CORE-A}       & 6 &59457\pm364 & 750_{-153}^{+337}&{\rm A}\\[0.5mm]
{\rm CORE-B}       & 6 &57493\pm434 & 894_{-597}^{+290}&{\rm B}\\[0.5mm]
{\rm Passive\ gals}       & 34 &57325\pm252 & 
1447_{-152}^{+247}&^{{\rm b}}{\rm C,D}\\[0.5mm]
{\rm Active\ gals}       &14  &58950\pm411 & 
1462_{-440}^{+704}&{\rm A}\\[0.5mm]
{\rm Balmer\ abs.\ gals}     & 9 &58988\pm668 & 1817_{-994}^{+834}&\\[0.5mm]
{\rm Emission\ lines\ gals } & 5 &58558\pm527 & 898_{-218}^{+363}&{\rm A}\\
             \noalign{\smallskip}
            \hline
         \end{array}
$$
\begin{list}{}{}  
\item[$^{{a}}$] We use the biweigth 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}). 
\item[$^{{b}}$] Notice that BCM-B resembles characteristics of 
a passive galaxy, but it does not appears in our classification
since its spectra has $\cal R$ slightly below the threshold value of~7. 
\end{list}
         \end{table}