Spitzer-IRAC GLIMPSE of high mass protostellar objects - II. SED modelling of a bona fide sample

J. M. C. Grave; M. S. N. Kumar

doi:10.1051/0004-6361/200810902

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Volume 498 / No 1 (April IV 2009)

A&A, 498 1 (2009) 147-159

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Issue		A&A Volume 498, Number 1, April IV 2009


Page(s)		147 - 159
Section		Interstellar and circumstellar matter
DOI		https://doi.org/10.1051/0004-6361/200810902
Published online		24 February 2009

Online Material

$\begin{figure} \par\includegraphics[width=16cm,clip]{figure1_near1.eps} \end{figure}$	Figure 1: Observed SED and their best fit models. Filled circular symbols represent the data points and the filled triangles represent photometry used as upper limits on the fitting. The dashed line corresponds to the stellar photosphere model used in the best YSO model fit.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=16cm,clip]{figure1_near2.eps} \end{figure}$	Figure 1: continued.
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$\begin{figure} \par\includegraphics[width=16cm,clip]{figure1_near3.eps} \end{figure}$	Figure 1: continued.
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$\begin{figure} \par\includegraphics[width=16cm,clip]{figure1_far1.eps} \end{figure}$	Figure 1: continued.
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$\begin{figure} \par\includegraphics[width=16cm,clip]{figure1_far2.eps} \end{figure}$	Figure 1: continued.
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$\begin{figure} \par\includegraphics[width=16cm,clip]{figure1_far3.eps} \end{figure}$	Figure 1: continued.
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Table 1: Parameters obtained for all the sources in our sample.

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