All Figures

$\begin{figure} \par\includegraphics[width=14cm,clip]{1266fig1.eps} \end{figure}$ Figure 1: A typical sdB spectrum $T_{\rm eff}=32~000$ K, $\log g=5.8$ together with the SDSS filter transmission functions (labelled). The gap near the Balmer limit represents a region where hydrogen line opacity is not treated correctly by SPECTRUM.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1266fig2.eps} \end{figure}$ Figure 2: The photometric amplitude (in magnitudes) is plotted with the velocity amplitude for the passbands u' (triangle), g' (cross) and r' (diamond).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1266fig3.eps} \end{figure}$ Figure 3: The photometric amplitude ratio as a function of the wavelength for $\ell = 0$ (solid line), 1 (dotted line), 2 (dashed line), 3 (dashed dot line) and 4 (dashed dot dot dot line) in a model V361 Hya star of period 135 s and 185 s in the UBVR photometric system. We have shown the values of $\ell$ corresponding to the lines in the diagram.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1266fig4.eps} \end{figure}$ Figure 4: As Fig. 3 in the SDSS system. The bottom panel shows the effect of a small change in $T_{\rm eff}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1266fig5.eps} \end{figure}$ Figure 5: As Fig. 4 for a model PG 1716+426 star with periods of 40, 60 and 90 min.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1266fig6.eps} \end{figure}$ Figure 6: As Fig. 5 for a model PG 1716+426 star with periods of 40, 60 and 90 min in the UBVR system.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{1266fig1.eps} \end{figure}$	Figure 1: A typical sdB spectrum $T_{\rm eff}=32~000$ K, $\log g=5.8$ together with the SDSS filter transmission functions (labelled). The gap near the Balmer limit represents a region where hydrogen line opacity is not treated correctly by SPECTRUM.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1266fig2.eps} \end{figure}$	Figure 2: The photometric amplitude (in magnitudes) is plotted with the velocity amplitude for the passbands u' (triangle), g' (cross) and r' (diamond).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1266fig3.eps} \end{figure}$	Figure 3: The photometric amplitude ratio as a function of the wavelength for $\ell = 0$ (solid line), 1 (dotted line), 2 (dashed line), 3 (dashed dot line) and 4 (dashed dot dot dot line) in a model V361 Hya star of period 135 s and 185 s in the UBVR photometric system. We have shown the values of $\ell$ corresponding to the lines in the diagram.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1266fig4.eps} \end{figure}$	Figure 4: As Fig. 3 in the SDSS system. The bottom panel shows the effect of a small change in $T_{\rm eff}$ .
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1266fig5.eps} \end{figure}$	Figure 5: As Fig. 4 for a model PG 1716+426 star with periods of 40, 60 and 90 min.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1266fig6.eps} \end{figure}$	Figure 6: As Fig. 5 for a model PG 1716+426 star with periods of 40, 60 and 90 min in the UBVR system.
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