All Figures

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9696fig01.eps}}\end{figure}$ Figure 1: Twenty point sources visible in the 24 $\mu$ m MIPS image. Axes are in J2000 coordinates. The brightness scale is logarithmic, ranging from 27 (black), through red and yellow, to 170 MJy/sr (white). The ``S'' numbers correspond to the source IDs as listed in Table 1. The annuli around the brightest sources are artefacts of the instruments point spread function.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9696fig02.eps}}\end{figure}$ Figure 2: Composite image of IRDC G48.65. The color image is composed of images of the Spitzer passbands at 24 $\mu$ m (red), 8.0 $\mu$ m (green) and 4.5 $\mu$ m (blue). Overlaid are the 850 $\mu$ m SCUBA contours at levels of 0.08, 0.16, 0.24, 0.32 and 0.40 Jy/beam. The axes annotate right ascension and declination (J2000). Notable MIPS point sources are labeled.
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In the text

$\begin{figure} \par\mbox{\resizebox{4.4cm}{!}{\includegraphics{9696fig03a.eps}}\... ...ig03c.eps}}\resizebox{4.4cm}{!}{\includegraphics{9696fig03d.eps}} } \end{figure}$ Figure 3: Best fitting photosphere model (solid lines) to the data points (filled circles) of S4, S17, S18 and S19.
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In the text

$\begin{figure} \mbox{\includegraphics[width=6cm]{9696fig04a.eps}\includegraphics... ...ps}\hspace{8.85cm} \includegraphics[width=3.3cm]{9696fig04n.eps} } \end{figure}$ Figure 4: YSO model SEDs that fit best to the data points (filled circles) of thirteen sources. This figure shows those sources listed in Table 2. Objects S2, S5, S6, S7, S9 and S12 are discussed in detail in Sect. 3.2.1, objects S8, S11, S14 and S16 in Sect. 3.2.2 and objects S13 and S20 in Sect. 3.2.3. In each panel, the black or colored curve is the best fitting SED (if it is colored, this indicates dependence on aperture size, see legend in bottom right frame). The lighter shaded curves (gray or pale colors) are all other model SEDs for which the criterion in Eq. (2) is obeyed. The dashed curve is the photosphere used as input for the radiative transfer code that calculated the best fitting YSO SED.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9696fig05.eps}} \end{figure}$ Figure 5: Ranges of $\dot{M}_{\rm env}$ (vertical axis) and $M_{\rm disk}$ (horizontal axis) of models that fit the data of S6. The gray levels show the distribution of the models in the grid, where darker color indicates a higher density of models. The points show the loci of all models which obey the criterion in Eq. (2), i.e. the model SEDs which are plotted in Fig. 4.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9696fig06.eps}} \end{figure}$ Figure 6: Same as Fig. 5, for S8.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9696fig01.eps}}\end{figure}$	Figure 1: Twenty point sources visible in the 24 $\mu$ m MIPS image. Axes are in J2000 coordinates. The brightness scale is logarithmic, ranging from 27 (black), through red and yellow, to 170 MJy/sr (white). The ``S'' numbers correspond to the source IDs as listed in Table 1. The annuli around the brightest sources are artefacts of the instruments point spread function.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9696fig02.eps}}\end{figure}$	Figure 2: Composite image of IRDC G48.65. The color image is composed of images of the Spitzer passbands at 24 $\mu$ m (red), 8.0 $\mu$ m (green) and 4.5 $\mu$ m (blue). Overlaid are the 850 $\mu$ m SCUBA contours at levels of 0.08, 0.16, 0.24, 0.32 and 0.40 Jy/beam. The axes annotate right ascension and declination (J2000). Notable MIPS point sources are labeled.
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$\begin{figure} \par\mbox{\resizebox{4.4cm}{!}{\includegraphics{9696fig03a.eps}}\... ...ig03c.eps}}\resizebox{4.4cm}{!}{\includegraphics{9696fig03d.eps}} } \end{figure}$	Figure 3: Best fitting photosphere model (solid lines) to the data points (filled circles) of S4, S17, S18 and S19.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9696fig05.eps}} \end{figure}$	Figure 5: Ranges of $\dot{M}_{\rm env}$ (vertical axis) and $M_{\rm disk}$ (horizontal axis) of models that fit the data of S6. The gray levels show the distribution of the models in the grid, where darker color indicates a higher density of models. The points show the loci of all models which obey the criterion in Eq. (2), i.e. the model SEDs which are plotted in Fig. 4.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9696fig06.eps}} \end{figure}$	Figure 6: Same as Fig. 5, for S8.
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