\begin{table}%t9
\caption{\label{Fraction}Minimum and maximum equilibrium temperature and distribution of the dust mass with dust temperature ranges.}
\small%\centerline
 {
 \begin{tabular}{cc|ccc}
\hline
\hline
&&&& \\[-8pt]
\multicolumn{2}{c|}{}   & NGC~1705 $^a$& Haro~11 $^a$  & Mrk~1089\\
\hline
&&&& \\[-8pt]
\multicolumn{2}{c|}{$T_{\rm eq}$  $_{\rm (max)}$ (K) }    & 88.2&  125       & 146\\
\multicolumn{2}{c|}{$T_{\rm eq}$  $_{\rm (min)}$ (K)}   & 10&  10      & 16.9  \\
\multicolumn{2}{c|}{$f_{\rm mass}$ ([50 K; 150 K])}	 &   0.1${\%}$ 	&   0.4${\%}$ 		&   0.15${\%}$ \\
\multicolumn{2}{c|}{$f_{\rm mass}$ ([25 K; 50 K])}	 &   7.2${\%}$	&   28.9${\%}$ 		&   9.5${\%}$  \\
\multicolumn{2}{c|}{$f_{\rm mass}$ ([15 K; 25 K])}	 &   8.3${\%}$	&   0${\%}$ 	  	&   90.4${\%}$\\
\multicolumn{2}{c|}{$f_{\rm mass}$ (10 K) }	 		 &   84.4${\%}$&   70.4${\%}$   	&   0${\%}$\\
\hline
\end{tabular}}
\medskip
$^a$ The models used for NGC~1705 and Haro~11 include an independent, very cold dust component at 10~K with an emissivity $\beta$~=~1. 
\end{table}