\begin{table}%t3
%%\centering
\par
\caption{Parameters resulting from the best fits of stellar population models
to the photometric data for Sal, MS and Kro IMFs. The $\tilde\chi^2$ represent the 
reduced $\chi^2$. 
The model which formally provides the best fit (the lowest $\tilde\chi^2$) 
is marked with "*''. The $V$-band absolute magnitude has been derived by the $K$s-band
apparent magnitude. {The absolute magnitudes in the $K$s and in the $V$ bands
are corrected for the extinction.}}\label{t3}
 %\centerline
 {\begin{tabular}{llllcccccccc}
\hline
\hline
ID & SFH & $\tilde\chi^2$& P($\tilde\chi^2$)& $z_{\rm phot}$ & Age & $A_V$ & $Z$ &$M_V$& $M_K$ & $^aM$/$L_K$&$\mathcal{M}_{\rm stars}$\\
& &       &     &     & [Gyr] & [mag] & [$Z_\odot$]& [mag] &[mag]& [$M$/$L$]$_\odot$& [$10^{11}$$M_\odot$] \\ 
\hline
& Sal IMF  & & & & & & & & & &\\
HDFS\_1269$^*$&$\tau=0.3$   &0.33& 0.92& $\rm 2.4^{+0.3}_{-0.2}$& 2.0 & 0.3  & 0.4&$-$22.9& $-$25.1& 0.50& 1.2\\
HDFS\_822     &$\tau=0.3$   &0.06& 0.99& $\rm 3.0^{+0.3}_{-0.2}$& 1.7 & 1.0  & 0.2&$-$24.1& $-$26.1& 0.45& 3.3\\
HDFS\_850     &$\tau=0.1$   &0.16& 0.98& $\rm 2.9^{+0.2}_{-0.3}$& 0.5 & 1.9  & 1.0&$-$24.1& $-$25.8& 0.30& 1.4\\
\hline
& MS IMF  & & & & & & & & & &\\
HDFS\_1269    &$\tau=0.3$   &0.34& 0.92& $\rm 2.5^{+0.3}_{-0.2}$& 2.0 & 0.2  & 0.4&$-$22.9& $-$25.1& 0.26& 0.6\\
HDFS\_822$^*$ &$\tau=0.3$   &0.04& 0.99& $\rm 3.0^{+0.3}_{-0.2}$& 1.7 & 0.9  & 0.2&$-$24.1& $-$26.1& 0.23& 1.4\\
HDFS\_850     &$\tau=0.1$   &0.17& 0.98& $\rm 2.9^{+0.2}_{-0.3}$& 0.5 & 1.8  & 1.0&$-$24.0& $-$25.8& 0.14& 0.6\\
\hline
& Kro IMF  & & & & & & & & & &\\
HDFS\_1269    &$\tau=0.3$   &0.38& 0.89& $\rm 2.4^{+0.3}_{-0.2}$& 2.0 & 0.4  & 0.4&$-$22.9& $-$25.1& 0.38& 0.9\\
HDFS\_822     &$\tau=0.3$   &0.04& 0.99& $\rm 3.0^{+0.3}_{-0.2}$& 1.7 & 1.0  & 0.2&$-$24.1& $-$26.0& 0.35& 2.1\\
HDFS\_850$^*$ &$\tau=0.1$   &0.16& 0.98& $\rm 2.9^{+0.2}_{-0.3}$& 0.5 & 1.9  & 1.0&$-$24.0& $-$25.8& 0.22& 1.0\\
\hline
\end{tabular}
}
 {$^a$ We used $M_{\odot,K}=3.4$ (Allen \cite{All73}).}
\end{table}