\begin{table}%t2
%\centering
\par
\caption{Results of the stellar-mass estimate for the ellipticals sample, 
based of SEDs fitting with solar metallicity SSPs. For each elliptical 
source in the HDFS (Rodighiero et~al.  \cite{Rodighiero01}), spectroscopic (Vanzella et~al. \cite{Vanzella03}; 
Sawicky \& Mallen-Ornelas 2003) or photometric 
(if within parenthesis, Rodighiero) redshifts, total number 
of models produced by the spectrophotometric synthesis code, best fit parameters
and~$\chi^2$ for the analytic SFH method (see text for details),
mass of the best fit solution and~2$\sigma$ (95.5\% confidence) mass range due 
to degeneracies are reported. Third column reports a flag identifying red and
blue sources. The SEDs of the red sources have been fitted with three
different methods: {\em a)} analytic SFH, {\em b)} two simple stellar populations 
(10$^9$ and $1.2 \times  10^{10}$~yrs old) with solar metallicity, {\em c)} two old
populations ($1.2\times  10^{10}$~yrs) with different metallicities ($Z=0.02$, 0.008)  --
see also text and Fig.~\ref{fig:e_5}.
The mass ranges reported for these objects include the results of all three
fitting tecniques; on blue sources only the analytic SFH leads to good results.\label{tab:risultati_ellittiche}}
\begin{tabular}{l c c c c c c c c c c}
\hline
\hline
Obj & $z$ & Color &$N_{\rm tot}$ & $t_{\rm F}$ & $E(B-V)$ & $n_1$ & $\tau_1$ & $\chi^2$ & Mass (b.f.) & $\Delta M$ \\
\# & & Flag & mdls. & b.f. [Gyrs] & b.f. & b.f. & b.f. & b.f & $[10^{11}~M_\odot]$ & $[10^{11}~M_\odot]$ \\
\hline
E1  & 0.512   & b & 18~001 & 11.91& 0.05 & 2.69  & 0.16 & 8.67 & 0.18 & 0.08$-$0.18\\
E2  & (1.3)   & b & 16~848 & 11.66& 0.02 & 3.01  & 0.16 & 11.95& 0.83 & 0.47$-$1.07\\
E3  & (1.3)   & b & 23~427 & 3.44 & 0.05 & 4.12  & 0.08 & 7.95 & 0.85 & 0.70$-$1.82\\
E4  & 0.414   & b & 11~521 & 2.68 & 0.00 & 0.002 & 0.52 & 4.29 & 0.16 & 0.10$-$0.23\\
E5  & 0.673   & r & 129~606& 3.19 & 0.05 & 0.001 & 0.15 & 1.89 & 0.73 & 0.66$-$1.12\\
E6  & (0.5)   & r & 111~765& 9.20 & 0.06 & 0.002 & 0.15 & 6.31 & 0.90 & 0.52$-$1.16\\
E7  & 0.517   & b & 11~287 & 4.63 & 0.10 & 5.17  & 0.11 & 6.71 & 0.10 & 0.08$-$0.14\\
E8  & 0.579   & r & 131~529& 6.68 & 0.05 & 2.85  & 0.09 & 5.31 & 0.52 & 0.42$-$0.83\\
E9  & 0.515   & b & 15~841 & 2.00 & 0.00 & 5.25  & 0.10 & 6.68 & 0.05 & 0.045$-$0.059\\
E11 & 0.364   & r & 121~526& 7.17 & 0.04 & 2.35  & 0.06 & 9.92 & 0.10 & 0.07$-$0.16\\
E14 & (1.15)   & b & 11~053 & 11.44& 0.00 & 1.97  & 0.25 & 5.52 & 0.75 & 0.43$-$0.81\\
E16 & (1.0)   & b & 11~283 & 11.46& 0.05 & 0.04  & 0.26 & 8.36 & 3.42 & 2.29$-$3.99\\
E17 & (1.25)  & r & 136~281& 11.71& 0.04 & 0.03  & 0.19 & 7.31 & 3.89 & 2.82$-$4.08\\
E18 & (0.9)   & r & 112~240& 11.46& 0.04 & 0.02  & 0.19 & 4.58 & 0.73 & 0.38$-$0.89\\
E19 & (0.15)  & r & 121~521& 11.96& 0.05 & 3.98  & 0.01 & 9.81 & 0.08 & 0.06$-$0.09\\
E20 & (0.8)   & b & 16~087 & 2.00 & 0.00 & 0.001 & 0.34 & 9.76 & 0.12 & 0.08$-$0.18\\
E21 & 0.577   & r & 127~454& 11.28& 0.05 & 0.04  & 0.29 & 10.00& 0.98 & 0.61$-$1.16\\
E24 & (0.4)   & r & 134~001& 11.28& 0.05 & 3.35  & 0.08 & 13.54& 0.55 & 0.33$-$0.72\\
E25 & 0.511   & b & 13~272 & 11.97& 0.04 & 1.49  & 0.21 & 7.02 & 0.72 & 0.44$-$0.93\\
E26 & (1.5)   & b & 11~729 & 5.52 & 0.00 & 3.69  & 0.09 & 22.34& 2.80 & 1.89$-$4.12\\
E27 & (0.85)  & b & 11~258 & 11.72& 0.02 & 3.42  & 0.11 & 16.02& 0.92 & 0.52$-$1.09 \\
E28 & 0.564   & b & 11~281 & 11.91& 0.02 & 0.64  & 1.70 & 18.45& 0.13 & 0.086$-$0.14\\
E29 & (0.5)   & r & 112~123& 14.35& 0.05 & 2.76  & 0.01 & 4.79 & 0.18 & 0.078$-$0.32\\
\hline
\end{tabular}
\end{table}