\begin{table}%t2
\caption{\label{tbl:agefits}The disruption time and the formation rate of clusters 
within 600~pc from the Sun for two assumed values of the lower mass
limit of clusters in the Kharchenko et~al. (\cite{Kharchenko2005}) sample.}
%\centering
\par
\begin{tabular}{cccc}
\hline \hline 
Mass range & $\tgal$ & $\log~(CFR)$ & $\log~(CFR)$ \\
(\Msun)    &  (Myr)  & Nr/yr      &~\Msun/yr \\
\hline 
$8\times 10^1{-}1\times 10^5$ & $\rm 3.5^{+1.3}_{-1.0}$ &$-6.03\pm 0.02$ & $-3.27\pm 0.02$ \\
 %& & & \\
$1\times10^2{-}1\times 10^5$ & $\rm 3.1^{+1.2}_{-0.8}$ &$-6.03\pm 0.02$ & $-3.19\pm 0.02$ \\
\hline 
      adopted     & $\rm 3.3^{+1.4}_{-1.0}$ &$-6.03\pm 0.02$ & $-3.23\pm 0.06$ \\
\hline 
\end{tabular}
\end{table}