Table 4: Summary of parameters we used to fit the SEDs of the sources. We give their name and then the parameters themselves: the extinction in the optical Av, the temperature  $T_{\rm\ast }$ and the $\frac{R_{\rm \ast}}{D_{\rm \ast}}$ ratio of the star, and the temperature $T_{\rm D}$ and radius $R_{\rm D}$ (in $R_{\rm\ast }$ unit) of the dust component. We also add the reduced $\chi ^2$ we reach for each fit, as well as the uncertainties on the parameters.
Sources Av $T_{\rm\ast}[\Delta{T_{\rm\ast}}](\textrm{K})$ $\frac{R_{\rm \ast}}{D_{\rm \ast}}$ $T_{\rm D} (\textrm{K})$ $R_{\rm D}\left(R_{\ast}\right)$ $\chi^2/\textrm{d.o.f.}$
LBV 1806-20 (A) (2005) $\rm {28.6}_{-1.5}^{+1.5}$ 21 500 [17 900-26 200] $3.08_{-0.48}^{+0.36}\times10^{-{10}}$ $\rm 1130_{-110}^{+130}$ $\rm 8.4_{-0.9}^{+1.0}$ 3.1/4
LBV 1806-20 (A) (2006) $\rm 29.0_{-1.2}^{+1.2}$ 17 600 [15 000-21 200] $3.68_{-0.36}^{+0.24}\times10^{-{10}}$ $\rm 1020_{-100}^{+140}$ $\rm 6.5_{-0.7}^{+0.7}$ 3.9/4
WC9 (B) $\rm 35.2_{-1.8}^{+1.4}$ 53 000 [25 000-71 000] $4.36_{-0.68}^{+1.36}\times10^{-{11}}$ $\rm 1850_{-120}^{+60}$ $\rm 46.0_{-14.0}^{+8.0}$ 6.8/4
Supergiant (C) $\rm 31.8_{-2.1}^{+0.8}$ 25 700 [11 600-40 500] $1.38_{-0.36}^{+0.62}\times10^{-{10}}$     6.0/5


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