\begin{table}%t2
%\centering
\par
\caption{\label{tab2}Cross-Entropy fit parameters.} 
\begin{tabular}{lcccc}
\hline\hline
{Cluster} & {$V_{\rm cut}$} & {${\vec F}_{\rm star}$} & {3$\sigma_{\rm phot}$} & {Ref.} \\
&  {mag} & {$(\%)$} & {$(\%)$}  & \\
\hline
\object{NGC~2477}     &$17.00 $& $95$ &$ 1.0  $ & 152   \\ 
\object{NGC~2477}     &$17.00 $& $95$ &$ 1.0  $ & 152   \\ 
\object{NGC~7044}     &$21.75 $& $95$ &$ 1.0  $ &  62   \\
\object{NGC~2266}     &$18.75 $& $95$ &$ 1.5 $ & 41    \\
\object{Berkeley 32}  &$20.25 $& $95$ &$ 1.5  $ & 40    \\
\object{NGC~2682}     &$18.00 $& $98$ &$ 1.5 $ & 335   \\
&$18.00 $& $99$ &$ 1.5 $ & 31    \\
&$18.00 $& $98$ &$ 1.5 $ & 54    \\
\object{NGC~2506}     &$18.00 $& $98$ &$ 1.5  $ & 284   \\
             &$17.75 $& $98$ &$ 1.5 $ & 163   \\
\object{NGC~2355}     &$19.75 $& $98$ &$ 1.0  $ & 217   \\
             &$18.25 $& $98$ &$ 1.0  $ & 44    \\
\object{Melotte 105}  &$16.75 $& $98$ &$ 1.5  $ & 289   \\
             &$16.75 $& $98$ &$ 1.5  $ & 32    \\
\object{Trumpler 1}         &$19.00 $& $85$ &$ 1.5  $ & 320   \\ 
             &$19.00 $& $95$ &$ 1.5 $ & 86    \\
\hline
\end{tabular}
\tablefoot{$V_{\rm cut}$ is the adopted cut-off in magnitude in~$V$, $\rho_{\rm star}$ is the density of stars in the observed field as a function of radius determined from the cluster center and 3$\sigma_{\rm phot}$ is the photometric error as described in  the text.}\vspace*{-2mm}
\tablebib{152 =  \cite{Kassis1997}; 62  =  \cite{Aparicio1993}; 
41  =   \cite{Kaluzny1991}; 40~=~\cite{Kaluzny1991}; 
335 =  Henden 2003; 31~=~\cite{Gilliland1991};
54  =  \cite{Montgomery1993} (adopted $\log t = 9.6$);
284 =  \cite{Kim2001} (adopted mean values: see Table~5 of the paper);   
163 =  \cite{Marconi1997}; 217~=~\cite{Ann1999}; 44  =  \cite{Kaluzny1991}; 289 =  \cite{Sagar2001}; 32~=~\cite{Kjeldsen1991}; 320 =  \cite{Yadav2002}; 86  =  \cite{Phelps1994}.}
\end{table}