\begin{table}%T2
\caption{Predicted optical properties of the model galaxies.}\label{t2}
%\centerline
{
\begin{tabular}{lllllclll}
\hline
\hline
Model & ${\rm Mg_2}$ &        & $\langle$Fe$\rangle$ &        &
[$\langle$Mg/Fe$\rangle$] & $L_B$ & $L_K$\\%&$L_{\rm X}$ &$kT_X$\\
      &  T     & W      & T      & W     &         &($10^{10}~L_{\odot}$)&($10^{10}~L_{\odot}$)\\%&($10^{41}\rm erg/s$)&(keV) \\
\hline
L    &  0.301  &  0.232  &  3.00  &   2.68    &0.506  & 1.2&    7.7\\%  &     & \\
%La1   &  0.301  &  0.232  &  3.00  &   2.68    &0.506  &       1.2&    7.7\\%  &0.13 &0.87 \\
%La10  &  0.301  &  0.232  &  3.00  &   2.68    &0.506  &       1.2&    7.7\\%  &     & \\
H  &  0.304  &  0.220&    2.93  &  2.57  &  0.561  &    11.2&   80\\%&     &  \\
HSN1&0.431   & 0.350  &  3.94  &  3.78   &  0.462   & 18 &116 \\
HSN100&0.268   & 0.172  &  2.61  &  2.10   &  0.689   & 4.4 & 19.8\\
%Ha1   &  0.324  &  0.243&    3.10  &  2.78  &  0.528  &        1.1&    80\\%& 5.12&2.3 \\
%Ha10  &  0.324  &  0.243&    3.10  &  2.78  &  0.528  &        1.1&    80\\%&     &  \\
\hline
\end{tabular}}
\par
\medskip
The indices obtained with the Tantalo et~al.  (\cite{Tantalo98}) SSP are labelled with T, whereas W refers to the Worthey (\cite{Worthey94}) SSP (see text). 
The values presented here refer to the whole galaxy.
\end{table}