\begin{table}%t3
%\centering
\par
\caption{\label{t:tabratio}Original/final mass of GCs required to produce the observed ratios between number of stars in first and second generations.}
\begin{tabular}{lcccccc}
\hline\hline\noalign{\smallskip}
Prim/2nd gen&	IMF & $M_{\rm min}$&$M_{\rm max}$&Prim/2nd gen&	Original/Current&	Field/GCs\\
Current &	Slope	&  & &Original &&\\
(1)                       & (2)                   & (3)           &  (4)        & (5)         & (6) & (7) \\
\hline
\multicolumn{7}{c}{Massive AGB stars (HBB)}\\
0.5			&	1.35	& 4		& 8	 	&11.1	& 7.4	&	6.4 \\
0.5			&	1.85	& 4		& 8	 	&~9.7	& 6.5	&	5.5 \\
0.5			&	2.35	& 4		& 8		&15.8	& 10.6	&	9.6 \\
0.5			&	MS		& 4		& 8	 &~7.3	& 4.9	&	3.9 \\
\hline
\multicolumn{7}{c}{Fast rotating massive stars}\\
%\hline
0.5			&	1.35	& 12	&50	 	& 1.8	& 1.2	&	0.2 \\
0.5			&	1.85	& 12	&50	 	& 3.3	&	 2.2	&	1.2 \\
0.5			&	2.35	& 12	&50	 	&11.2	&	 7.5	&	6.5 \\
0.5			&	MS		& 12	&50	 &~3.0	&	 2.3	&	1.3 \\
\hline
\end{tabular}
\tablefoot{ 
\tablefoottext{1}{Current ratio between first and second generation stars;} 
\tablefoottext{2}{slope $\alpha$ of the IMF ($N(M)=M^{-\alpha}$; Salpeter (\cite{Salpeter1955}) IMF has $\alpha=2.35$; MS means that the IMF by Miller \& Scalo (\cite{Miller1979}) is adopted;} 
\tablefoottext{3}{Minimum polluter mass (in $M_\odot$);} 
\tablefoottext{4}{maximum polluter mass (in $M_\odot$);} 
\tablefoottext{5}{original ratio between first and second generation stars;} 
\tablefoottext{6}{ratio between the number of low-mass stars in the proto-cluster and in the current GC;} 
\tablefoottext{7}{current ratio of field stars (=primordial population lost by the cluster)
and of GC~stars. This is the value that can be compared with observational data.}}
\end{table}