\begin{table}%t1
\caption{\label{tbl:clusters_prop}Main properties of clusters in our sample.}
%\centerline
 {\small \begin{tabular}{lrrrrr}
\hline\hline\noalign{\smallskip}
ID &$\alpha$ (J2000) & $\delta$ (J2000) & $z$ & $L_X$ & $r_{200}$  \\ 
& & & & ($10^{-37}$ $W$) &  (Mpc)\\  
\noalign{\smallskip}
\hline
MS 0015.9+1609  & 00:18:33.33  & +16:26:44.6 & 0.54 [2] & 15.5 [2]  & 2.11 [3]\\ 
MS 0451.5-0305  & 04:54:10.796 & --03:00:53.0 & 0.54 [2] & 23.7 [2] & 1.47 [3]\\ 
MS 1621.5+2640  & 16:23:35.6277 & +26:34:09.49 & 0.43 [2] & 9.47 [2]  & 1.5 [3]\\ 
MS1241.5+1710  & 12:44:01.4 & +16:53:42 & 0.55 [2] & 1.73 [2] & 1.7 [3]\\ 
RXC J0856.1+3756   & 08:56:08.5 &+37:56:52  & 0.41 [1] & 15.76 [1] & 1.59 [3]\\ 
RX J1003.0+3757  & 10:03:02.74 & +37:57:51.5 & 0.41 [1] & 8.29 [1] & 1.48 [3]\\ 
RX J1120+4318   & 11:20:07.5 & +43:18:05 & 0.60 [2] & 6.07 [2] &  1.3 [3]\\ 
RXC J1206.2-0848  & 12:06:13.1  & --08:47:43 & 0.44 & -- &  2.0 [3]\\ 
RXC J2228.6+2036  & 22:28:37.1 & +20:36:31& 0.41 [1] & 29.62 [1] &  1.62 [3]\\ 
\hline
\end{tabular}}
\medskip
[1] \cite{Bohringer00}; [2]~\cite{Sadat04}; [3]~Foex et~al. 2009, in prep. $r_{200}$ are computed through a 1D~weak-lensing analysis, i.e. fit of the radial shear profile and are defined as the radius at which the density is 200 times the critical density of the Universe at the cluster redshift.
\end{table}