All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{10934fg1.eps} \end{figure}$ Figure 1: MIDI and ISO/SWS flux of the source in the mid-infrared. Dotted line with $\sim$ 10% error bars is the 2005 MIDI flux from the UTs ( $\phi \sim 0.75$ ); dashed line with $\sim$ 10% error bars is the 2006 MIDI flux from the UTs ( $\phi \sim 0.30$ ); dashed dot dot dot line with $\sim$ 25% error bars is the 2007 MIDI flux from the ATs ( $\phi \sim 0.00$ ). The two solid lines are the ISO/SWS spectra (upper one: 1996, $\phi =0.65$ ; bottom one: 1997, $\phi =0.08$ ).
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In the text

$\begin{figure} \par {\hspace*{7.5mm}\includegraphics[width=6cm,clip]{10934fg2.ep... ...space*{7.5mm}}\\ \includegraphics[width=13.5cm,clip]{10934fg4.eps} \end{figure}$ Figure 2: Top-left: best-fit model of the single dust shell spectrum (thin line) supperimposed on the ATs MIDI flux (error bars), the 2 ISO/SWS spectra (upper thick line: 1996, $\phi =0.65$ , and bottom thick line: 1997, $\phi =0.08$ ), and the photometric data (open triangles) with (U/B/V/R/J/H/K/L/M/N) data from Yudin et al. (1994) and I band from Chochol et al. (2004). Top-right: close-up view of the best-fit model to the dust feature. Bottom: the corresponding model visibility (solid line) superimposed on the MIDI visibilities (error bars) for the eleven projected baselines.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{10934fg5.eps} \end{figure}$ Figure 3: Calibrated differential phase of the object evaluated from all the determined ATs projected baselines (dotted lines). Error bars correspond to the rms of the differential phase averaged over all the projected baselines. The bold solid line is the central value of these error bars.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{10934fg6.eps} \end{figure}$ Figure 4: Spectrally-dispersed uv coverage of the 2005-2006-2007 observations from 8 to 12.5 $\mu$ m.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{10934fg7.eps} \end{figure}$ Figure 5: Brightness distribution of the best-fit elliptical Gaussian model of HM Sge from 8 to 12.5 $\mu$ m (north is up and east is left).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{10934fg8.eps}\includegraphics[width=8cm,clip]{10934fg9.eps} \end{figure}$ Figure 6: Left: full width at half maximum of the major axis for the best-fit elliptical Gaussian model as a function of wavelength. Right: ratio of the minor to the major axis for the best-fit elliptical Gaussian model as a function of wavelength.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{10934fg5.eps} \end{figure}$	Figure 3: Calibrated differential phase of the object evaluated from all the determined ATs projected baselines (dotted lines). Error bars correspond to the rms of the differential phase averaged over all the projected baselines. The bold solid line is the central value of these error bars.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{10934fg6.eps} \end{figure}$	Figure 4: Spectrally-dispersed uv coverage of the 2005-2006-2007 observations from 8 to 12.5 $\mu$ m.
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$\begin{figure} \par\includegraphics[width=18cm,clip]{10934fg7.eps} \end{figure}$	Figure 5: Brightness distribution of the best-fit elliptical Gaussian model of HM Sge from 8 to 12.5 $\mu$ m (north is up and east is left).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{10934fg8.eps}\includegraphics[width=8cm,clip]{10934fg9.eps} \end{figure}$	Figure 6: Left: full width at half maximum of the major axis for the best-fit elliptical Gaussian model as a function of wavelength. Right: ratio of the minor to the major axis for the best-fit elliptical Gaussian model as a function of wavelength.
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