$\begin{figure} \par\includegraphics[width=17.6cm,clip]{8892fig2.ps} \end{figure}$ Figure 2: Molecular emission detected with APEX and JCMT in the S-type AGB W Aql. Note that the HCN(9-8) line is rebinned to a resolution of 3.6 km s^-1, other lines are rebinned to a resolution of 1.8 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.9cm,clip]{8892fig5.ps}\hspa... ...ace*{0.4cm} \includegraphics[angle=90,width=7.9cm,clip]{8892fig8.ps}\end{figure}$ Figure 5: The structure of the CSE as derived using the GASTRoNOoM-code is shown for the four studied targets WX Psc, W Aql, II Lup, and V Cyg. Since the focus is on the inner and intermediate regions, only the first 200 $R_{\star }$ are displayed. Upper panel: estimated temperature profile, middle panel: estimated gas velocity structure, and bottom panel: estimated hydrogen density $n_{{\rm H_2}}$ . The dashed line indicates the dust condensation radius, $R_{{\rm inner}}$ . The variable mass-loss rate of WX Psc, mostly noticeable in the hydrogen density, is discussed in Decin et al. (2007).
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In the text

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{8892fig1.ps} \end{figure}$	Figure 1: Molecular emission detected with APEX and JCMT in the O-rich AGB WX Psc.
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$\begin{figure} \par\includegraphics[width=17.6cm,clip]{8892fig2.ps} \end{figure}$	Figure 2: Molecular emission detected with APEX and JCMT in the S-type AGB W Aql. Note that the HCN(9-8) line is rebinned to a resolution of 3.6 km s^-1, other lines are rebinned to a resolution of 1.8 km s^-1.
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$\begin{figure} \par\includegraphics[angle=90,width=14.5cm,clip]{8892fig3.ps} \end{figure}$	Figure 3: Molecular emission detected with APEX in the C-rich AGB II Lup.
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$\begin{figure} \par\includegraphics[angle=90,width=14.5cm,clip]{8892fig4.ps} \end{figure}$	Figure 4: Molecular emission detected with JCMT in the C-rich AGB V Cyg.
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