All Figures

$\begin{figure} \includegraphics[width=13cm]{0388fig1.eps} \end{figure}$ Figure 1: a) Top. A position-switched high-resolution CO J=2-1 spectrum toward IRAS 16594-4656. Bottom. A beam-switched CO J=3-2 spectrum toward IRAS 16594-4656. b) Top. A position-switched high-resolution CO J=2-1 spectrum toward IRAS 17150-3224. Bottom. A beam-switched CO J=3-2 spectrum toward IRAS 17150-3224.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{0388fi2a.eps}\hspace*{4mm} \includegraphics[width=8cm]{0388fi2b.eps} \end{figure}$ Figure 2: Position-position contour emission maps of IRAS 16594-4656, and IRAS 17150-3224. Blue contours show blue-shifted emission, black contours emission from the centre of the line profile, and red contours red-shifted emission.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=14cm,clip]{0388fig3.eps} \end{figure}$ Figure 3: A map of the CO J=2-1 line around IRAS 16954-4656. The beam-spacing is 11 $^{\prime \prime }$ . The spectra are affected by interstellar line contamination in the red-shifted line wing.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=14cm,clip]{0388fig4.eps} \end{figure}$ Figure 4: A map of the CO J=2-1 line around IRAS 17150-3224, taken in beamswitch mode. The beam-spacing is 11 $^{\prime \prime }$ . The spectra are affected by interstellar line contamination in the blue-shifted line wing.
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In the text

$\begin{figure} \includegraphics[width=11cm,clip]{0388fig5.eps} \end{figure}$ Figure 5: CO J=2-1 spectra of PPNe candidates, named in the upper left-hand corner of each spectrum.
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In the text

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{0388fig6.eps} \end{figure}$ Figure 6: Best fit CO model of IRAS 16594-4656 (solid line) overlayed on observations (histogram) using a mass loss rate of $1\times 10^{-5}$ $M_{\odot }$ yr^-1 and a ¹²CO/¹³CO-ratio of 30.
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In the text

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{0388fig7.eps} \end{figure}$ Figure 7: Best fit CO model of IRAS 17150-3224 (solid line) overlayed on observations (histogram) using a mass loss rate of $3\times 10^{-5}$ $M_{\odot }$ yr^-1 and a ¹²CO/¹³CO-ratio of 7.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=17cm,clip]{0388fig8.eps} \end{figure}$ Figure 8: Results of the chemical model of IRAS 16594-4656. The figure shows the variation of the fractional abundances (or ratios, in the lower row of axes) of selected species radially through the expanding circumstellar envelope at different points in time (measured in years since the cessation of mass-loss). The shading marks the passage of the inner edge of the circumstellar envelope. As can be seen at long times (5000 yr), only CO is reasonably abundant. The three sets of axes labelled "0 yr'' show the results of a standard AGB model (see Sect. 6.3.2).
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{0388fig9.eps} \end{figure}$ Figure A.1: Molecular line observations of IRAS 16594-4656.

In the text

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{0388fi10.eps} \end{figure}$ Figure A.2: Molecular line observations of IRAS 16594-4656.

In the text

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{0388fi11.eps} \end{figure}$ Figure A.3: Molecular line observations of IRAS 17150-3224.

In the text

$\begin{figure} \includegraphics[width=13cm]{0388fig1.eps} \end{figure}$	Figure 1: a) *Top. A position-switched high-resolution CO J=2-1 spectrum toward IRAS 16594-4656. Bottom. A beam-switched CO J=3-2 spectrum toward IRAS 16594-4656. b) Top. A position-switched high-resolution CO J=2-1 spectrum toward IRAS 17150-3224. Bottom*. A beam-switched CO J=3-2 spectrum toward IRAS 17150-3224.
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$\begin{figure} \par\includegraphics[width=8cm]{0388fi2a.eps}\hspace*{4mm} \includegraphics[width=8cm]{0388fi2b.eps} \end{figure}$	Figure 2: Position-position contour emission maps of IRAS 16594-4656, and IRAS 17150-3224. Blue contours show blue-shifted emission, black contours emission from the centre of the line profile, and red contours red-shifted emission.
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$\begin{figure} \par\includegraphics[angle=270,width=14cm,clip]{0388fig3.eps} \end{figure}$	Figure 3: A map of the CO J=2-1 line around IRAS 16954-4656. The beam-spacing is 11 $^{\prime \prime }$ . The spectra are affected by interstellar line contamination in the red-shifted line wing.
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$\begin{figure} \par\includegraphics[angle=270,width=14cm,clip]{0388fig4.eps} \end{figure}$	Figure 4: A map of the CO J=2-1 line around IRAS 17150-3224, taken in beamswitch mode. The beam-spacing is 11 $^{\prime \prime }$ . The spectra are affected by interstellar line contamination in the blue-shifted line wing.
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$\begin{figure} \includegraphics[width=11cm,clip]{0388fig5.eps} \end{figure}$	Figure 5: CO J=2-1 spectra of PPNe candidates, named in the upper left-hand corner of each spectrum.
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$\begin{figure} \par\includegraphics[width=17.5cm,clip]{0388fig6.eps} \end{figure}$	Figure 6: Best fit CO model of IRAS 16594-4656 (solid line) overlayed on observations (histogram) using a mass loss rate of $1\times 10^{-5}$ $M_{\odot }$ yr^-1 and a ¹²CO/¹³CO-ratio of 30.
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$\begin{figure} \par\includegraphics[width=17.5cm,clip]{0388fig7.eps} \end{figure}$	Figure 7: Best fit CO model of IRAS 17150-3224 (solid line) overlayed on observations (histogram) using a mass loss rate of $3\times 10^{-5}$ $M_{\odot }$ yr^-1 and a ¹²CO/¹³CO-ratio of 7.
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