\begin{table}%t2
\caption{\label{tab:local}Properties of the local cluster sample from Vikhlinin et~al. (2006).}
%\centerline
 {\begin{tabular}{ccccc}
\hline \hline
 Cluster & $z$ & $kT_{\rm gas}$ &  $R_{500}$ & $f_{\rm gas}$ \\ 
  &  &  keV & kpc & ($<$$R_{500}$) \\
\hline 
A133 & 0.057 & $4.15\pm0.07$ & $1027\pm38$ & $0.087\pm0.006$ \\
A1795 & 0.062 & $6.10\pm0.06$ & $1320\pm47$ & $0.108\pm0.006$ \\
A2029 & 0.078 & $8.46\pm0.09$ & $1419\pm32$ & $0.128\pm0.007$ \\
A478 & 0.088 & $7.95\pm0.14$ & $1398\pm62$ & $0.125\pm0.011$ \\
A1413 & 0.143 & $7.38\pm0.12$ & $1377\pm49$ & $0.112\pm0.007$ \\
A907 & 0.160 & $5.96\pm0.08$ & $1149\pm32$ & $0.129\pm0.006$ \\
A383 & 0.188 & $4.80\pm0.12$ & $983\pm34$ & $0.129\pm0.007$ \\
A2390 & 0.230 & $8.90\pm0.17$ & $1489\pm50$ & $0.147\pm0.009$ \\
\hline 
\end{tabular}}
\medskip
 Column (1): name; Col.~(2): adopted redshift; Col.~(3): best-fit spectral temperature;
Col.~(4): $R_{500}$; Col.~(5): gas mass fraction within $R_{500}$. A cosmology of $(H_0, \Omega_{\rm m}, \Omega_{\Lambda}) = (70$~km~s$^{-1}$~Mpc$^{-1},
0.3, 0.7)$ is adopted here.
\end{table}