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Figure 1:
MIDI and ISO/SWS flux of the source in the mid-infrared. Dotted line with ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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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, ![]() ![]() |
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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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Figure 4:
Spectrally-dispersed uv coverage of the 2005-2006-2007 observations from 8 to 12.5 ![]() |
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Figure 5:
Brightness distribution of the best-fit elliptical Gaussian model of HM Sge from 8 to 12.5 ![]() |
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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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