\begin{table}%t2
\caption{TDGs progenitors. }
\label{tab:TDGs}
%\centerline
{
\begin{tabular}{llcccc}
\hline \hline
Run & Location & $T$ $^a$ & $M_{\rm tot}$ $^b$ & $M_{\rm *}^{\rm old}$ $^c$ & $M_{\rm *}^{\rm young}$ $^d$\\
     & & (Myr) & (\Mo) & (\%) & (\%) \\
\hline
A & $x>0$ & 60 & $2.9 ~\x~ 10^9$ & 5\% & 19\% \\
   & $x<0$ &    & $2.3 ~\x~ 10^9$ & 12\% & 13\% \\
   & $x>0$ & 430 & $2.2 ~\x~ 10^9$ &  5\%  & 44\%  \\
   & $x<0$ &   & $1.8 ~\x~ 10^9$ & 14\% &  31\% \\ \hline
B  & $x<0$ & 100 & $2.3 ~\x~ 10^9$ &  7\%  & 19\%  \\ \hline
C & $x>0$ & 90 & $2.5 ~\x~ 10^{9}$ $^e$ &  11\%  & 16\%  \\
   & $x<0$ &  & $1.8 ~\x~ 10^9$ &  11\%  & 16\%  \\ \hline
D & $y>0$ & 55 & $1.1 ~\x~ 10^9$ &  3\%  & 14\%  \\
   & $y<0$ & & $2.4 ~\x~ 10^9$ &  8\%  & 19\%  \\ 
\hline
\end{tabular}}
\medskip
$^a$ Time after the periapse.  \\
$^b$ Total mass.  \\
$^c$ Mass of the old stellar population from the parent's disk.  \\
$^d$ Mass of the young stellar population born in situ. Note that this value is approximate as the measurement of the SFR is affected by the limited numerical resolution.  \\
$^e$ In two fragments.  \\
\end{table}