\begin{table}%t2online
\caption{\label{tab:fit}SED fit parameters and results.}
\begin{tabular}{llllllllll}%{lcccccccccc}
\hline \hline \noalign{\smallskip}
&$T_*$&$L_*$&$T_{\rm in}$&$R_*$&$R_{\rm out}/R_{\rm in}$&$R_{\rm in}$&
$\dot{M}_{\rm total}$& $T_{\rm dust}^{\rm sub-mm}$ & $M_{\rm dust}^{\rm sub-mm}$ \\
&($10^4$~K)&($10^5~L_\odot$)&(K)& ($R_\odot$) & & (km) & ($M_\odot~{\rm yr}^{-1}$)& (K) & ($M_\odot$) \\
\hline\noalign{\smallskip}
R71 (inner/outer shell)& $1.5$ & $4.6$ &490/120&100&2/1.6&$\sim$$10^{11}$/$10^{12}$&$\sim$$10^{-6}$ / $\sim$$10^{-4}$ & $9 \pm 1$ & $\gtrsim$$10^{-1}$ \\
IRAS05280$-$6910&0.3&$2.2$&250&1700&30&$\sim$$10^{11}$&$\sim$$10^{-3}$ &...&... \\ 
HD~36402& $18$ & $4.6$ &960&15&300&$\sim$$10^{10}$&$7\times10^{-6}$ &...&... \\
HD~36402 IR1 (YSO2)&...&...&...&...&...&...&...&$64$/$15$ ($\pm 1$) & $10^{-12}$/$>$$1.5 \pm 0.4$\\ 
\hline
\end{tabular}
\tablefoot{Fitting results from 2-D{\sc ust}.  {\sc dusty}
fits for R71 and IRAS05280-6910 estimate outer shell MLRs 2$\times$ to
4$\times$ less than the 2-D{\sc ust} results.  IR1/YSO2 was fit with
two modified blackbodies (64~K and 15~K). For R71, we use O-deficient
silicate optical constants \citep{ossenkopf92} at long wavelengths and
astronomical silicate optical constants \citep{draine84} at $\lambda <
0.18$~\micron{}. For IRAS05280--6910, we use \citet{ossenkopf92}
O-deficient silicates and for HD~36402, we use amorphous carbon
grains from \citet{zubko96}. The 2-D{\sc ust} models use a KMH grain
size distribution \citep*{kim94} with $a_{\rm min}=0.01~\micron$ and
$a_0=0.1~\micron$ ($a_0=1~\micron$ for IRAS05280-6910). Stellar
parameters for R71 are consistent with those from
\citet{lennon93}. $T_{\rm dust}^{\rm sub-mm}$ is the temperature of
the coldest dust component. For IRAS5280-6910, $\upsilon_{\rm
wind}$ is measured from the maser emission
\citep[20~km~s$^{-1}$;][]{marshall04}. For R71, we use
10~km~s$^{-1}$, but the velocity measured from the H$\alpha$ profile
indicates the inner shell velocity may be $>$10$\times$ larger
\citep{stahl86}. For HD36402, a typical velocity for a WC4 star is
assumed \citep[3000~km~s$^{-1}$;][]{willis04}.}
\end{table}