\begin{table}%t8
\caption{\label{ISRF_dwarfs}Dust masses derived from SED models using different shapes of ISRFs.}
\small%\centerline
 {
\begin{tabular}{c|ccc|ccc|cc}
\hline
\hline
&&&&&&&& \\[-8pt]
Synthesized ISRF  &  \multicolumn{3}{c|}{NGC~1705 $^a$}  &\multicolumn{3}{c|}{Haro~11 $^a$} & \multicolumn{2}{c}{Mrk~1089}  \\
 \multicolumn{1}{c|}{ }  & $M_{\rm warm}$ $_{\rm dust}$ $^b$ &  $M_{\rm dust}$ $^c$ &  $\bar{\chi}$$^2$ & $M_{\rm warm}$ $_{\rm dust}$ $^b$ &  $M_{\rm dust}$ $^c$ &  $\bar{\chi}$$^2$ & $M_{\rm dust}$ & $\bar{\chi}$$^2$ \\
\hline
&&&&&&&& \\[-8pt]
Milky Way				 & 2.6 $\times$ 10$^4$&   	   1.7 $\times$ 10$^5$	& 2	& 5.9 $\times$ 10$^6$ &		2 $\times$ 10$^7$	      & 13 	& 	5.2 $\times$ 10$^7$  & 5.7\\
Non-ionising cluster		 & 2.5 $\times$ 10$^4$&	   1.7 $\times$ 10$^5$  	& 5	& 6.5 $\times$ 10$^6$  &		2.1 $\times$ 10$^7$        & 25 	& 	5.0 $\times$ 10$^7$  	   & 21\\
He 2-10				 & 3.3 $\times$ 10$^4$&	   1.75 $\times$ 10$^5$ 	& 20	& 8.7 $\times$ 10$^6$  &		2.19 $\times$ 10$^7$      & 45 	& 	7.0 $\times$ 10$^7$  & 52\\
IIZw40				 & 2.8 $\times$ 10$^4$&	   1.71 $\times$ 10$^5$ 	& 12	& 8.7 $\times$ 10$^6$  &		2.24 $\times$ 10$^7$      & 36 	& 	4.9 $\times$ 10$^7$  & 41\\
NGC 1140				& 2.8 $\times$ 10$^4$&	   1.72 $\times$ 10$^5$ 	& 12	& 8.1 $\times$ 10$^6$   &		2.2 $\times$ 10$^7$        & 38 	& 	4.7 $\times$ 10$^7$  & 46 \\
NGC 1569				& 2.6 $\times$ 10$^4$&   	   1.69 $\times$ 10 $^5$ 	& 2	& 6.6 $\times$ 10$^6$  &		2.02 $\times$ 10$^7$      & 14 	& 	5.0 $\times$ 10$^7$        & 16\\
\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. \\
$^b$ $M_{\rm warm}$ $_{\rm dust}$ is the dust mass without including the 10~K dust mass (but with cold dust included in the fit). \\
$^c$ $M_{\rm dust}$ is the total dust mass of the galaxy, 10~K dust mass included for Haro~11.
\end{table}