All Figures

$\begin{figure} \par\includegraphics[width=9cm]{4585fg1.ps} \end{figure}$ Figure 1: F435W HST/ACS image of the young planetary nebula CPD-56 $^\circ$ 8032 with the HRC (resolution 0.027 $\hbox {$^{\prime \prime }$ }$ pixel^-1). A logarithmic stretch has been used. North is up, East is left.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm]{4585fg2.eps} \end{figure}$ Figure 2: Sketch of the HST F435W nebula. The dynamic scale has been highly exaggerated in order to enhance the remarkable structures which are labeled in the figure.
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In the text

$\begin{figure} \par\mbox{\includegraphics[height=6.2cm, width=7.5cm]{4585fg3.ps}\qquad \includegraphics[height=6.2cm, width=7.5cm]{4585fg4.ps} } \end{figure}$ Figure 3: Left: the MIDI spectrum of CPD-56 $^\circ$ 8032 (lower solid) is shown in comparison to the ISO one (upper solid). A MIDI spectrum scaled to the ISO one is also presented (dotted line) to ease the comparison of the PAH features. The transmission of the 8.7 $~\mu$ m filter used for the target acquisition is also shown (dashed). The continuum fit of the ISO spectrum (upper dashed-dotted) is based on the parameters described in Cohen et al. (2002). The fit of the MIDI spectrum (lower dashed-dotted) is based on a slight modification of these parameters (see in text). Right: the result of ratio of the ISO (solid line) and MIDI (dashed line) with their respective approximate continua, showing further the clear discrepancy between the two curves.
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In the text

$\begin{figure} \par\includegraphics[width=5.2cm, angle=-90]{4585fg5.ps}\par\incl... ...585fg6.ps}\par\includegraphics[width=5.2cm, angle=-90]{4585fg7.ps} \end{figure}$ Figure 4: MIDI dispersed visibilities (solid lines, CPD1 to CPD3 from top to bottom) and the best analytical monochromatic models of an inclined disk (Gaussian ring, dotted lines). The $\chi ^2$ for the three baselines are 4.3, 1.8 and 14.3 respectively.
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In the text

$\begin{figure} \par\includegraphics[width=5.4cm, angle=-90]{4585fg11.ps}\vspace*... ...pace*{3.4mm} \includegraphics[width=5.4cm, angle=-90]{4585fg10.ps} \end{figure}$ Figure 5: One of the best models with single chemistry. Top: the ISO spectrum (solid line) is compared with the model SED (dotted line). The MIDI flux (dashed line) is very close to the model one (within 10%, small dotted line). The $\chi ^2$ for the three baselines are 7.5, 3.9 and 10.4 respectively.
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In the text

$\begin{figure} \par\includegraphics[width=9cm]{4585fg1.ps} \end{figure}$	Figure 1: F435W HST/ACS image of the young planetary nebula CPD-56 $^\circ$ 8032 with the HRC (resolution 0.027 $\hbox {$^{\prime \prime }$ }$ pixel^-1). A logarithmic stretch has been used. North is up, East is left.
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$\begin{figure} \par\includegraphics[width=7.5cm]{4585fg2.eps} \end{figure}$	Figure 2: Sketch of the HST F435W nebula. The dynamic scale has been highly exaggerated in order to enhance the remarkable structures which are labeled in the figure.
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$\begin{figure} \par\includegraphics[width=5.2cm, angle=-90]{4585fg5.ps}\par\incl... ...585fg6.ps}\par\includegraphics[width=5.2cm, angle=-90]{4585fg7.ps} \end{figure}$	Figure 4: MIDI dispersed visibilities (solid lines, CPD1 to CPD3 from top to bottom) and the best analytical monochromatic models of an inclined disk (Gaussian ring, dotted lines). The $\chi ^2$ for the three baselines are 4.3, 1.8 and 14.3 respectively.
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$\begin{figure} \par\includegraphics[width=5.4cm, angle=-90]{4585fg11.ps}\vspace... ...pace{3.4mm} \includegraphics[width=5.4cm, angle=-90]{4585fg10.ps} \end{figure}$	Figure 5: One of the best models with single chemistry. Top: the ISO spectrum (solid line) is compared with the model SED (dotted line). The MIDI flux (dashed line) is very close to the model one (within 10%, small dotted line). The $\chi ^2$ for the three baselines are 7.5, 3.9 and 10.4 respectively.
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