Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=17.25cm,clip]{1490fig1.ps} \end{figure}$ Figure 1: Left panel: spectral energy distribution for the post-MS star HD 41511. Mid panel: the corresponding TIMMI2 N-band spectrum. Right panel: decomposition of the dust emission. The different linestyles represent small amorphous olivine ( dotted), large amorphous olivine ( dashed), silica (SiO₂, dash-dotted) and crystalline forsterite ( dash-three dots).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.45cm,clip]{1490fig2.ps} \end{figure}$ Figure 2: Spectral energy distributions for our Vega-type sources. A Kurucz model is overplotted to represent the stellar contribution to the SED. The mm-fluxes are upper limits, as indicated by the arrow.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.45cm,clip]{1490fig3.ps} \end{figure}$ Figure 3: TIMMI2 spectra of the Vega-type stars. For some objects the data between approximately 9.0 and 9.7 $\mu$ m is taken out, as there was a detector problem in the 2002 run. Smaller gaps between about 9.4 and 9.7 $\mu$ m occur where we cut out uncorrectable atmospheric ozone features.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{1490fig4.ps} \end{figure}$ Figure 4: Left panel: decomposition into dust components for HD 113766. Right panel: similar analysis for HD 172555. The different linestyles represent small amorphous olivine ( dotted), large amorphous olivine ( dashed), silica (SiO₂, dash-dotted) and crystalline forsterite ( dash-three dots).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1490fig5.ps} \end{figure}$ Figure 5: Comparison of HD 113766 with comet Hale-Bopp and the Herbig Be star HD 100546 (both scaled in y-direction). The resemblance is remarkable and demonstrates that HD 113766 has similar dust characteristics as those objects. In contrast, AB Aur, a young HAe star with very little processed dust is shown in the bottom panel.
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In the text

$\begin{figure} \par\includegraphics[width=17.25cm,clip]{1490fig1.ps} \end{figure}$	Figure 1: Left panel: spectral energy distribution for the post-MS star HD 41511. Mid panel: the corresponding TIMMI2 N-band spectrum. Right panel: decomposition of the dust emission. The different linestyles represent small amorphous olivine ( dotted), large amorphous olivine ( dashed), silica (SiO₂, dash-dotted) and crystalline forsterite ( dash-three dots).
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=8.45cm,clip]{1490fig2.ps} \end{figure}$	Figure 2: Spectral energy distributions for our Vega-type sources. A Kurucz model is overplotted to represent the stellar contribution to the SED. The mm-fluxes are upper limits, as indicated by the arrow.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=8.45cm,clip]{1490fig3.ps} \end{figure}$	Figure 3: TIMMI2 spectra of the Vega-type stars. For some objects the data between approximately 9.0 and 9.7 $\mu$ m is taken out, as there was a detector problem in the 2002 run. Smaller gaps between about 9.4 and 9.7 $\mu$ m occur where we cut out uncorrectable atmospheric ozone features.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=14cm,clip]{1490fig4.ps} \end{figure}$	Figure 4: Left panel: decomposition into dust components for HD 113766. Right panel: similar analysis for HD 172555. The different linestyles represent small amorphous olivine ( dotted), large amorphous olivine ( dashed), silica (SiO₂, dash-dotted) and crystalline forsterite ( dash-three dots).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1490fig5.ps} \end{figure}$	Figure 5: Comparison of HD 113766 with comet Hale-Bopp and the Herbig Be star HD 100546 (both scaled in y-direction). The resemblance is remarkable and demonstrates that HD 113766 has similar dust characteristics as those objects. In contrast, AB Aur, a young HAe star with very little processed dust is shown in the bottom panel.
Open with DEXTER