\begin{table}%t3
\caption{\label{SEDtable}Results of the spectral energy distribution fitting without dust and 
with dust models of various types.}
%\centerline
 {\small  
\begin{tabular}{lcccc}
\hline\hline\noalign{\smallskip}
Dust model   & Redshift$^1$ & $\beta^1$ & $A_V^{\rm host}$  & $\chi^2_{\rm red}$ \\
&          &         & (mag)        &  \\    
\hline
none & $\rm 4.35^{+0.12}_{-0.13}$ & $\rm 0.38^{+0.20}_{-0.19}$ & --  & 1.04  \\
Milky Way   & $\rm 4.35^{+0.12}_{-0.16}$ & $\rm 0.38^{+0.21}_{-0.23}$ & $\rm 0.0^{+0.4}_{-0.0}$ &1.04\\
Large Magellanic Cloud  & $\rm 4.28^{+0.15}_{-0.24}$ & $\rm 0.34^{+0.19}_{-0.24}$ & $\rm 0.1^{+0.4}_{-0.1}$ &0.95\\
Small Magellanic Cloud  & $\rm 4.35^{+0.13}_{-0.26}$ & $\rm 0.38^{+0.13}_{-0.28}$ & $\rm 0.0^{+0.2}_{-0.0}$ &1.04\\
\hline
\end{tabular}}
\medskip
$^1$ Errors are at the 2$\sigma$ confidence level. 
\end{table}