All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{5078fig1.ps} \end{figure}$ Figure 1: From bottom to top: the light curves in the EPIC PN 0.2-15 keV range, in the B band, and in the UV 2000-2800 $\AA$ range binned in 50 s.
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In the text

$\begin{figure} \par\includegraphics[height=8cm,width=7.3cm,angle=-90,clip]{5078fig2.ps} \end{figure}$ Figure 2: EPIC-PN power spectra in selected energy ranges. From bottom to top: 0.2-15 keV, 0.2-0.5 keV, 0.5-1 keV, 1-2 keV, 2-5 keV, and 5-12 keV. The spin ( $\omega$ ) and harmonics, the beat ( $\omega - \Omega$ ), and the orbital ( $\Omega$ ) frequencies as derived from optical data (Burwitz et al. 1996) are marked with vertical dotted lines. Inserted panels show an enlargement around the spin frequency ( lower panel) and the spectral window of the data.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{5078fig3a.ps}\hspace*{4mm} \includegraphics[width=6.4cm,clip]{5078fig3b.ps} \end{figure}$ Figure 3: Left: EPIC-PN folded light curves in selected energy bands at the 863.3 s period using the ephemeris quoted in the text. Right: the EPIC hardness ratios show the complex energy dependence of the pulse.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,height=6.2cm,clip]{5078fig4.ps} \end{figure}$ Figure 4: The 0.2-0.5 keV EPIC PN folded light curve at the 3.55 h orbital period.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,height=7.8cm,clip]{5078fig5.ps} \end{figure}$ Figure 5: The 0.2-0.5 keV spin light curves extracted at orbital maximum ( lower panel) and orbital minimum ( upper panel).
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,height=7.8cm,clip]{5078fig6.ps} \end{figure}$ Figure 6: The UV 2000-2800 AA ( upper panel) and the B band spin folded light curves showing the strong colour dependence of pulsation.
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In the text

$\begin{figure} \par\includegraphics[height=6.4cm,width=6.3cm,angle=-90,clip]{5078fig7.ps} \end{figure}$ Figure 7: The EPIC PN ( top) and combined MOS ( bottom) spectra fitted simultaneously with Model A (see text). The bottom panel shows the ratio between observed and model spectra.
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In the text

$\begin{figure} \par\includegraphics[width=7.cm,height=7.2cm,clip]{5078fig8.ps} \end{figure}$ Figure 8: The RGS spectra (RGS1 in black and RGS2 in gray), along with Model A, derived from the EPIC spectral analysis. The positions of lines expected to be strong are also reported. The ratio between model and observed spectra is shown in the lower panel.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5078fig1.ps} \end{figure}$	Figure 1: From bottom to top: the light curves in the EPIC PN 0.2-15 keV range, in the B band, and in the UV 2000-2800 $\AA$ range binned in 50 s.
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{5078fig3a.ps}\hspace*{4mm} \includegraphics[width=6.4cm,clip]{5078fig3b.ps} \end{figure}$	Figure 3: Left: EPIC-PN folded light curves in selected energy bands at the 863.3 s period using the ephemeris quoted in the text. Right: the EPIC hardness ratios show the complex energy dependence of the pulse.
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$\begin{figure} \par\includegraphics[width=7.2cm,height=6.2cm,clip]{5078fig4.ps} \end{figure}$	Figure 4: The 0.2-0.5 keV EPIC PN folded light curve at the 3.55 h orbital period.
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$\begin{figure} \par\includegraphics[width=6.8cm,height=7.8cm,clip]{5078fig5.ps} \end{figure}$	Figure 5: The 0.2-0.5 keV spin light curves extracted at orbital maximum ( lower panel) and orbital minimum ( upper panel).
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$\begin{figure} \par\includegraphics[width=6.8cm,height=7.8cm,clip]{5078fig6.ps} \end{figure}$	Figure 6: The UV 2000-2800 AA ( upper panel) and the B band spin folded light curves showing the strong colour dependence of pulsation.
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$\begin{figure} \par\includegraphics[height=6.4cm,width=6.3cm,angle=-90,clip]{5078fig7.ps} \end{figure}$	Figure 7: The EPIC PN ( top) and combined MOS ( bottom) spectra fitted simultaneously with Model A (see text). The bottom panel shows the ratio between observed and model spectra.
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$\begin{figure} \par\includegraphics[width=7.cm,height=7.2cm,clip]{5078fig8.ps} \end{figure}$	Figure 8: The RGS spectra (RGS1 in black and RGS2 in gray), along with Model A, derived from the EPIC spectral analysis. The positions of lines expected to be strong are also reported. The ratio between model and observed spectra is shown in the lower panel.
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