All Figures

$\begin{figure} \par\includegraphics[width=5.7cm,clip]{1989fig1.ps}\hspace*{3mm} ... ...ig5.ps}\hspace*{3mm} \includegraphics[width=5.7cm,clip]{1989fig6.ps}\end{figure}$ Figure 1: The SEDs of 6 RV Tauri stars: the dereddened fluxes are given together with the scaled photospheric Kurucz model representing the unattenuated stellar photosphere (solid line). An optically thin dust fit was used to model the IR excess (dotted line). Data found in the literature together with our 7 band Geneva photometry (only the maxima) are plotted as triangles. The minimal data points (squares) were not used for the determination of E(B-V). They are only plotted to give an idea of the amplitude of the pulsations. Crosses represent our $850~\mu$ m SCUBA data point. Error bars on the $850~\mu$ m SCUBA data point are plotted as well, though for some objects smaller than the symbols. The arrow at the $100~\mu$ m fluxpoint shows that this data point is an upper limit for some stars.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{1989fig7.ps}\end{figure}$ Figure 2: The SED of R Sct is clearly different from these of the other programme stars. Symbols are the same as in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{1989fig7.ps}\end{figure}$	Figure 2: The SED of R Sct is clearly different from these of the other programme stars. Symbols are the same as in Fig. 1.
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