\begin{table}%t2
        \caption{Results of kinematical and spatial analysis.}
         \label{tabsub}
 %\centerline
{        \begin{tabular}{l r l l}
            \hline
            \hline 
${\rm Sample}$ & ${N_{\rm g}}$ & $\phantom{249}{\langle V \rangle }\phantom{249}$ & 
$\phantom{24}\sigma_{\rm V}^{~~~~~~~{a}}\phantom{24}$\\
& &$\phantom{249}{\rm km\ s}^{-1}\phantom{249} $
&$\phantom{2}{\rm km\ s}^{-1}\phantom{24}$\\
            \hline
            \noalign{\smallskip}
 ${\rm Whole\ system}$ & 85 &$91~754\pm192 $&$\rm 1767_{-99}^{+121}$\\
\hline
${\rm KMM\ partitions}$&&\\
${\rm KMMa}$ & 66 &$90~939\pm161 $&$\rm 1301_{-84}^{+130}$\\
${\rm KMMb}$ & 19 &$94~846\pm110 $&$\phantom{1}462_{-55}^{+58}$\\ 
${\rm KMM3Da}$& 57 &$90~616\pm156 $&$\rm 1170_{-100}^{+116}$\\
${\rm KMM3Db}$& 28 &$94~370\pm163 $&$\phantom{1}841_{-108}^{+177}$\\
\hline
${\rm 2D\ subsamples}$&&\\
$R<0.4{\rm \ Mpc, low}\ V$& 23 &$90~537\pm180 $&$\phantom{1}841_{-169}^{+319}$\\
$R<0.4{\rm \ Mpc, high}\ V$&12&$94~821\pm195$&$\phantom{1}631_{-103}^{+233}$\\
$R>0.4{\rm \ Mpc, N}   $& 32 &$91~262\pm238$ &$\rm 1319_{-118}^{+176}$\\
$R>0.4{\rm \ Mpc, S}   $& 18 &$93~081\pm476$ &$\rm 1940_{-317}^{+467}$\\
$R>0.4{\rm \ Mpc, W}   $& 36 &$91~793\pm276$ &$\rm 1628_{-143}^{+206}$\\
$R>0.4{\rm \ Mpc, E}   $& 14 &$91~676\pm500$ &$\rm 1779_{-189}^{+276}$\\
$R>0.4{\rm \ Mpc, NW}  $& 24 &$91~311\pm278$ &$\rm 1325_{-146}^{+218}$\\
\hline
${\rm Dressler\ \&\ Schectman\ substructure}$&&\\
${\rm DS, low}\ V$& 17 &$89~932\pm202 $&$\phantom{1}798_{-104}^{+142}$\\
${\rm DS, high}\ V$&11&$94~046\pm269$&$\phantom{1}834_{-114}^{+157}$\\
\hline
         \end{tabular}}
\medskip
\par
$^{{a}}$ 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{table}