\begin{table}%T7
\par
\caption{\label{dered}Fitting parameters of the SED of the IRS~13 sources.  The
spectral type of each source, as discussed in Sect.~\ref{nature}, is
summarized in the last column.}
%\begin{center}
{
\begin{tabular}{ l | l  r  r  r l | c }
\hline\hline
Star & {\it Coef$_1$} & ${T}_{1}$~K & {\it Coef$_2$} &
  ${T}_{2}$~K & ~$A_{\rm v}$ &{Sp. type} \\
\hline
W  &{13.50} &{3600}          &{4250} &{640}&          38.5&M3III  \\
E1 &{0.800} &{$\geq$25~000} &{12~000} &{550}& 35&$\sim$O5I \\
E2 &{0.620} &{$\geq$25~000} &{40~000} &{550}& 35& $\sim$WN8\\
E4 &{0.140} &{$\geq$25~000} &{45} &{1550}&35&$\sim$O5IIIe \\
E3A &{0.460} &{3800}         &{33~000} &{610}& 35& d. WR$^a$ \\
E3B &{0.375} &{3800}         &{29~000} &{580}& 35& d. WR$^a$ \\
E5 &{0.070} &{6000}          &{9800} &{630}  & 35& d. WR$^a$ \\
E6 &{0.013} &{$\geq$25~000} & &                & 29& $\sim$O5V   \\
\hline
   \end{tabular}}\\[2mm]
\parbox{8.5cm}{
$^a$ Dusty Wolf-Rayet star.}
%\end{center}
\par
\end{table}