\begin{table}%t3
\par
\caption {\label{tab:clump_props}Properties of the clumps. 
}
%\centerline
 {
\begin{tabular}{lllllll}
\hline\hline
           & $N_{\rm spec. member}$ & $z$                  & $\sigma$  [$\rm km s^{-1}$] & $R_{200}$ [Mpc]         & $M_{200}$ [$M_\odot$]            & $P_{\rm bound}$\\
\hline 
RDCSJ1252 cluster & 38 & $\rm 1.2370_{-0.0011}^{+0.0009}$ & $\rm 754_{ -89}^{ +55}$         & $\rm 0.93_{-0.11}^{+0.07}$  & $\rm 3.7_{-1.1}^{+0.9}\times10^{14}$ & -- \\\vspace{2pt}
Clump~1    & 5         & $\rm 1.2365_{-0.0015}^{+0.0002}$  & $\rm  44_{  -5}^{+271}$         & $\rm 0.05_{-0.01}^{+0.33}$  & $\rm 7.6_{-2.5}^{+270}\times10^{11}$ & $\rm 86^{ +7}_{-36}$\\\vspace{2pt}
Clump~2a   & 6         & $\rm 1.2135_{-0.0013}^{+0.0010}$  & $\rm 287_{-159}^{ +36}$         & $\rm 0.36_{-0.20}^{+0.04}$  & $\rm 2.1_{-1.9}^{+0.9}\times10^{13}$ & $\rm  0^{ +0}_{ -0}$\\\vspace{2pt}
Clump~2b   & 10        & $\rm 1.2343_{-0.0013}^{+0.0012}$  & $\rm 517_{-164}^{ +97}$         & $\rm 0.64_{-0.20}^{+0.12}$  & $\rm 1.2_{-0.8}^{+0.8}\times10^{14}$ & $\rm 51^{+28}_{-28}$\\\vspace{2pt}
Clump~3a   & 8         & $\rm 1.1748_{-0.0019}^{+0.0015}$  & $\rm 435_{-200}^{ +32}$         & $\rm 0.55_{-0.25}^{+0.04}$  & $\rm 7.3_{-6.2}^{+1.7}\times10^{13}$ & $\rm  0^{ +0}_{ -0}$\\\vspace{2pt}
Clump~3b   & 8         & $\rm 1.2350_{-0.0008}^{+0.0005}$  & $\rm 235_{ -94}^{ +41}$         & $\rm 0.29_{-0.12}^{+0.05}$  & $\rm 1.1_{-0.9}^{+0.7}\times10^{13}$ & $\rm 47^{+28}_{-27}$\\\vspace{2pt}
Clump~4    & 2         & $1.1745$                      & --                          & --                      & --                               & $\rm 0^{+0}_{-0}$\\
\hline
\end{tabular}}
\smallskip
The second column shows the number of spectroscopically 
confirmed members in each clump. Redshifts (3rd~column) and velocity dispersions 
(4th~column) are estimated with the biweight estimator \citep{beers90}.
The redshift errors are estimated by bootstrapping,
taking into account individual redshift errors.
The~5th and 6th~columns show the Virial radii and masses \citep{carlberg97}.
The last column shows the probability that each clump is dynamically bound to
RDCSJ1252. The galaxies in clump2a are not spatially concentrated,
suggesting that this clump probably not a bound system. There are only two members in clump~4 and the redshift is an average redshift of these two galaxies. The properties 
of RDCSJ1252 are added for reference. See text for details.
\end{table}