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$\begin{figure} \par\includegraphics[angle=90,width=18cm,clip]{2510fig1.eps} \end{figure}$ Figure 1: New observations of CO and HCN radio line emission.
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In the text

$\begin{figure} \par\includegraphics[width=17.3cm,clip]{2510fig2.eps} \end{figure}$ Figure 2: Observed SEDs for the seven carbon stars with detected detached molecular shells. Best-fit models to the observed SEDs are overlayed (solid line). The model SEDs are composed of a stellar part (dashed line), a present-day wind (dotted line), and a detached shell (dash-dotted line). The model SEDs have been corrected for interstellar extinction. Stellar and envelope parameters are summarized in Tables 3 and 4.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{2510fig3.eps}\end{figure}$ Figure 3: $\chi ^2$ -maps showing the sensitivity of the adjustable parameters $T_{{\rm dust}}$ and $M_{{\rm dust}}$ in the dust modelling of the detached shells around DR Ser and TT Cyg. Contours are drawn at $\chi ^2_{{\rm min}} + (2.3, 6.2, 11.8)$ indicating the 68% ("1 $\sigma$ ''), 95% ("2 $\sigma$ ''), and 99.7% ("3 $\sigma$ '') confidence levels, respectively. The quality of the best fit model can be estimated from the reduced chi-squared statistic $\chi ^{2}_{{\rm red}}$ = $\chi ^{2}_{{\rm min}}$ /(N-2) shown in the upper right corner.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{2510fig4.eps}\end{figure}$ Figure 4: The shell dust ( $M_{{\rm dust}}$ ; upper panel) and gas ( $M_{{\rm gas}}$ ; lower panel) masses plotted as a function of the radius of the shell ( $R_{\rm s}$ ). Note that the gas and dust shell radii are determined independently (see also Fig. 10). The solid line shows the mass-radius relation of the interacting wind model presented in Sect. 6.2.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{2510fig5.eps}\end{figure}$ Figure 5: $\chi ^2$ -maps showing the sensitivity of the adjustable parameters $n_{{\rm H_2}}$ , $T_{{\rm kin}}$ , and $R_{\rm s}$ in the CO modelling of the detached shell around V644 Sco. Contours are drawn at $\chi ^2_{{\rm min}} + (2.3, 6.2, 11.8)$ indicating the 68% ("1 $\sigma$ ''), 95% ("2 $\sigma$ ''), and 99.7% ("3 $\sigma$ '') confidence levels, respectively. The quality of the best fit model can be estimated from the reduced chi-squared statistic $\chi ^{2}_{{\rm red}}$ = $\chi ^{2}_{{\rm min}}$ /(N-2) shown in the lower left corner. Also indicated is the value of the parameters that is kept fixed in these maps.
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In the text

$\begin{figure} \par\includegraphics[width=16.25cm,clip]{2510fig6.eps} % \end{figure}$ Figure 6: Best fit models (solid line) including both the present-day wind and detached shell emission overlayed on observed spectra (histograms) for U Ant and U Cam. The uncertainty in the intensity scale is $\pm$ 20%. The narrow spikes found near the blue wing in the spectra of U Cam are of interstellar origin.
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In the text

$\begin{figure} \par\includegraphics[width=7.15cm,clip]{2510fig7.eps}\end{figure}$ Figure 7: The present-day-wind gas expansion velocity ( upper panel) and mass-loss rate ( lower panel) plotted as a function of the radius of the shell ( $R_{\rm s}$ ).
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{2510fig8.eps} \end{figure}$ Figure 8: The shell expansion velocity ( $V_{{\rm s}}$ ) plotted against the shell radius ( $R_{\rm s}$ ; as determined from CO line data). The solid line shows the expected velocity-radius relation of the interacting wind model presented in Sect. 6.2.
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{2510fig9.eps} \end{figure}$ Figure 9: The dust-to-gas ratio ( $\Psi$ ) plotted against the radius of the shell ( $R_{\rm s}$ ; assuming that the dust and gas shells coincide spatially).
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In the text

$\begin{figure} \par\includegraphics[width=6.65cm,clip]{2510fig10.eps} \end{figure}$ Figure 10: Relation between the radius of the shell as determined from dust and gas modelling, respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=18cm,clip]{2510fig1.eps} \end{figure}$	Figure 1: New observations of CO and HCN radio line emission.
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$\begin{figure} \par\includegraphics[width=6.7cm,clip]{2510fig4.eps}\end{figure}$	Figure 4: The shell dust ( $M_{{\rm dust}}$ ; upper panel) and gas ( $M_{{\rm gas}}$ ; lower panel) masses plotted as a function of the radius of the shell ( $R_{\rm s}$ ). Note that the gas and dust shell radii are determined independently (see also Fig. 10). The solid line shows the mass-radius relation of the interacting wind model presented in Sect. 6.2.
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$\begin{figure} \par\includegraphics[width=16.25cm,clip]{2510fig6.eps} % \end{figure}$	Figure 6: Best fit models (solid line) including both the present-day wind and detached shell emission overlayed on observed spectra (histograms) for U Ant and U Cam. The uncertainty in the intensity scale is $\pm$ 20%. The narrow spikes found near the blue wing in the spectra of U Cam are of interstellar origin.
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$\begin{figure} \par\includegraphics[width=7.15cm,clip]{2510fig7.eps}\end{figure}$	Figure 7: The present-day-wind gas expansion velocity ( upper panel) and mass-loss rate ( lower panel) plotted as a function of the radius of the shell ( $R_{\rm s}$ ).
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$\begin{figure} \par\includegraphics[width=6.7cm,clip]{2510fig8.eps} \end{figure}$	Figure 8: The shell expansion velocity ( $V_{{\rm s}}$ ) plotted against the shell radius ( $R_{\rm s}$ ; as determined from CO line data). The solid line shows the expected velocity-radius relation of the interacting wind model presented in Sect. 6.2.
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$\begin{figure} \par\includegraphics[width=6.7cm,clip]{2510fig9.eps} \end{figure}$	Figure 9: The dust-to-gas ratio ( $\Psi$ ) plotted against the radius of the shell ( $R_{\rm s}$ ; assuming that the dust and gas shells coincide spatially).
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$\begin{figure} \par\includegraphics[width=6.65cm,clip]{2510fig10.eps} \end{figure}$	Figure 10: Relation between the radius of the shell as determined from dust and gas modelling, respectively.
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