\begin{table}%t4
%\centering
\par
\caption{Summary of the syntheses of the internal region obtained for different settings for the non stellar parameters. In the first column, BB means "blackbody'', PL "power law'', $D$ corresponds to the synthetic distance obtained. (1) the lower bound of the $E(B-V)$ parameter is fixed to 0.8, (2) same as the previous one with upper bound for the contribution of the power law fixed to 30\%, (3) same as the first one with the blackbody temperature fixed to 1200~K. The constraint parameters are indicated in bold font.}
\label{res_nuc}
\small
\begin{tabular}{lccccc}
\hline\hline
Spectral Type       & lifetime (year)       &    1           &    2                &    3                    \\
\hline
A0V                 & $2\times10^8$         & 0\%            & 0\%                 & 0\%                     \\
F0IV                & $2\times10^9$         & 0\%            & 0\%                 & 0\%                     \\
F2V                 & $10^9$           & 0\%            & 0\%                 & 0\%                     \\
rG1V                & $4\times10^9$         & 0\%            & 3.0\%               & 0\%                     \\
G1.5V               & $6\times10^9$         & 0\%            & 0\%                 & 0\%                     \\
rG4V                & $10^{10}$        & 0\%            & 10.0\%              & 0\%                     \\
K0V                 & $2\times10^{10}$      & 0\%            & 0\%                 & 0\%                     \\
K3V                 & $3\times10^{10}$      & 0\%            & 0\%                 & 0\%                     \\
rK3V                & $3\times10^{10}$      & 6.2\%            & 0\%                 & 1.0\%                     \\
K4V                 & $4\times10^{10}$      & 0\%            & 0\%                 & 0\%                     \\
wK5V                & $4\times10^{10}$      & 0\%            & 0\%                 & 0\%                     \\
M0V                 & $\geq$$4\times10^{10}$ & 0\%            & 0\%                 & 0\%                     \\
rM1V                & $\geq$$4\times10^{10}$ & 2.1\%            & 0\%                 & 5.3\%                     \\
M1.5V               & $\geq$$4\times10^{10}$ & 17.2\%         & 19.7\%              & 18.2\%                  \\
M3V                 & $\geq$$4\times10^{10}$ & 0\%          & 24.9\%              & 11.0\%                  \\
\hline
F3III               & $2\times10^{9}$       & 0\%            & 0\%                 & 0\%                     \\
F8III               & $10^9$           & 0\%            & 0\%                 & 0\%                     \\
wG6III              & $8\times10^{9}$       & 0\%            & 0\%                 & 0\%                     \\
K1III               & $7\times10^{9}$       & 0\%            & 0\%                 & 0\%                     \\
K3III               & $6\times10^{9}$       & 0\%            & 0\%                 & 0\%                     \\
K5-M0III            & $6\times10^{9}$       & 0\%            & 0\%                 & 0\%                     \\
M1IIIab             & $5\times10^{9}$       & 0\%            & 0\%                 & 0\%                     \\
M4III               & $3\times10^{9}$       & 74.5\%         & 42.5\%              & 64.6\%                  \\
\hline
F0I                 & $10^7$           & 0\%            & 0\%                 & 0\%                     \\
F5I                 & $10^7$           & 0\%            & 0\%                 & 0\%                     \\
rF8Ib               & $10^7$           & 0\%            & 0\%                 & 0\%                     \\
G0Ib                & $2\times10^{7}$       & 0\%            & 0\%                 & 0\%                     \\
rK2I                & $10^7$           & 0\%            & 0\%                 & 0\%                     \\
K4I                 & $10^7$           & 0\%            & 0\%                 & 0\%                     \\
M2I                 & 2--$8\times10^6$       & 0\%            & 0\%                 & 0\%                     \\
\hline
\hline
Stellar contrib.    & & 19.1\%         & 29.6\%              & 21.0\%           \\
BB ($T_{\rm{eff}}$) & & 2.4\% (300 K)   & 40.4\% (1500 K)      & 22.7\% \textbf{(1200 K)} \\
PL ($\alpha_{\nu}$) & & 78.5\% (0.5)   & \textbf{30\%} (0.5) & 56.3\% (0.5)            \\
$E(B-V)$              & & \textbf{0.8}   & \textbf{0.8}        & \textbf{0.8}            \\
\hline
\hline
$D$                   & & $1.55\times10^{-4}$ & $1.84\times10^{-4}$      & $1.77\times10^{-4}$          \\
\hline
\end{tabular}
\end{table}