All Figures

$\begin{figure} \par\includegraphics[height=15.5cm, angle=-90,clip=]{7013_fig1.ps}\end{figure}$ Figure 1: The light curves of MU Cam, obtained simultaneously on March 31, 2005, by XMM (PN and OM) and with the AIP 70 cm-telescope (R). The data shown here are binned in time, 60 s for the first, second, and forth panel (counted from top to bottom), 120 s for the lower two. The R-band data are unbinned.
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In the text

$\begin{figure} \par\includegraphics[height=15.5cm, angle=-90,clip=]{7013_fig2.ps}\end{figure}$ Figure 2: The light curves of MU Cam, obtained on April 6, 2006, by XMM (PN, MOS1, MOS2, and OM). The data shown here are binned to 120 s.
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In the text

$\begin{figure} \par\includegraphics[height=8.8cm, angle=-90,clip]{7013_fig3a.eps... ...ip\\ \includegraphics[height=8.8cm, angle=-90,clip]{7013_fig3b.eps}\end{figure}$ Figure 3: Top: R-band light curve from May 8, 2006, bottom: the above data with BJED $\le$ 2453864.56, binned into 20 bins on the spin period calculated with the ephemeris given by Staude et al. (2003). The error bars mark the standard deviation of the values entering each bin.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,angle=0,clip=]{7013_fig4a.eps}\par\includegraphics[width=8.8cm,angle=0,clip=]{7013_fig4b.eps}\end{figure}$ Figure 4: The EPIC X-ray spectra from 2005 ( top) and 2006 ( bottom) (green PN, red+black: MOS1/2) with overplotted fit and residuals (Parameters in Table 2). The insets show an enlarged view of the iron-K region.
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In the text

$\begin{figure} \par\includegraphics[height=8.8cm,angle=-90,clip=]{7013_fig5.eps}\end{figure}$ Figure 5: The spectral energy distribution of MU Cam. Shown are the data synchronously obtained in 2005 (rhombs and X-ray model spectrum in black), the data from 2006 (XMM-Newton: circle and X-ray model spectrum in red, R-band flux from the 70 cm telescope: triangle), and, additionally, 2MASS J, H, and K fluxes ( squares) plus the optical spectra from Araujo-Betancor et al. (2003) ( lower) and Wei et al. (1999) ( upper). Additionally, the three data points from the INTEGRAL/IBIS spectrum (Barlow et al. 2006) are plotted with their corresponding error bars. The X-ray models are plotted without the interstellar absorption component. To illustrate the shape of the black body component in the X-rays, the extrapolation to lower energies outside the fitted range is plotted with dots.
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In the text

$\begin{figure} \includegraphics[angle=-90,width=8.5cm,clip]{7013_fig6a.eps}\hspace*{2.5mm} \includegraphics[angle=-90,width=8.5cm,clip]{7013_fig6b.eps}\end{figure}$ Figure 6: AOV-periodograms of left: the data from 2005 (Fig. 1) - PN counts in different energy ranges, OM with UVM2, and R-band photometry - for comparison, the AOV analysis of the R-band data from 2003 (Staude et al. 2003) is added; right: the data from 2006 (Fig. 2) in different energy ranges and instruments. The orbital ( $\Omega$ ) and spin ( $\omega$ ) frequencies, their sidebands, and (sub-)harmonics are marked with dotted lines.
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In the text

$\begin{figure} \par\includegraphics[height=8.8cm,angle=-90,clip]{7013_fig7a.eps}... ...m} \par\includegraphics[height=8.8cm,angle=-90,clip]{7013_fig7b.eps}\end{figure}$ Figure 7: The background-subtracted PN count rate in the energy band MHX (700 to 12 000 eV) ( top 2005/03/31, bottom 2006/04/06) binned to 30 s, plotted over spin-phase ( upper). The same data, binned into 50 phase bins with an overplotted spline fit ( lower).
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In the text

$\begin{figure} \par\mbox{\includegraphics[height=13.5cm,angle=0,clip]{7013_fig8a... ...9mm} \includegraphics[height=13.5cm,angle=0,clip]{7013_fig8b.eps} } \end{figure}$ Figure 8: The spin-folded PN light curves from for 700-12 000 eV ( MHX) and 200-700 eV ( SX). For the calculation of the spin-phase, we use as zero points the epochs of maximum flux in the MHX band determined in Sect. 4.2 and the period from Staude et al. (2003). The error bars in the light curves mark the standard deviation of the values having entered the bin. Below are plotted the spin-phase dependent parameter values for the fit to phase-selected MOS+PN spectra. The parameters not shown here were kept constant at the values determined from the fit to the average spectrum. Left: March 31, 2005, right: April 06, 2006.
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In the text

$\begin{figure} \par\includegraphics[height=13.57cm,angle=0,clip]{7013_fig9.eps}\end{figure}$ Figure 9: Light curves in the hard and soft X-ray bands from 2005 folded on the period corresponding to $\omega -\Omega /2$ (error bars in the light curves are the standard deviation of the values having entered the bin), and the free parameters of the fits to the phase-resolved spectra.
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In the text

$\begin{figure} \par\includegraphics[height=13.5cm,angle=0,clip]{7013_fig10.eps}\end{figure}$ Figure 10: The orbital period $\Omega$ : light curves from 2005 in the hard and soft X-ray bands, the fitted spectral parameters, and the phase-folded R-band data. The error bars of the light curves are the standard deviation of the values having entered the bin.
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In the text

$\begin{figure} \par\includegraphics[height=15.5cm, angle=-90,clip=]{7013_fig1.ps}\end{figure}$	Figure 1: The light curves of MU Cam, obtained simultaneously on March 31, 2005, by XMM (PN and OM) and with the AIP 70 cm-telescope (R). The data shown here are binned in time, 60 s for the first, second, and forth panel (counted from top to bottom), 120 s for the lower two. The R-band data are unbinned.
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$\begin{figure} \par\includegraphics[height=15.5cm, angle=-90,clip=]{7013_fig2.ps}\end{figure}$	Figure 2: The light curves of MU Cam, obtained on April 6, 2006, by XMM (PN, MOS1, MOS2, and OM). The data shown here are binned to 120 s.
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$\begin{figure} \par\includegraphics[height=8.8cm, angle=-90,clip]{7013_fig3a.eps... ...ip\\ \includegraphics[height=8.8cm, angle=-90,clip]{7013_fig3b.eps}\end{figure}$	Figure 3: Top: R-band light curve from May 8, 2006, bottom: the above data with BJED $\le$ 2453864.56, binned into 20 bins on the spin period calculated with the ephemeris given by Staude et al. (2003). The error bars mark the standard deviation of the values entering each bin.
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$\begin{figure} \par\includegraphics[width=8.8cm,angle=0,clip=]{7013_fig4a.eps}\par\includegraphics[width=8.8cm,angle=0,clip=]{7013_fig4b.eps}\end{figure}$	Figure 4: The EPIC X-ray spectra from 2005 ( top) and 2006 ( bottom) (green PN, red+black: MOS1/2) with overplotted fit and residuals (Parameters in Table 2). The insets show an enlarged view of the iron-K region.
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$\begin{figure} \par\includegraphics[height=8.8cm,angle=-90,clip]{7013_fig7a.eps}... ...m} \par\includegraphics[height=8.8cm,angle=-90,clip]{7013_fig7b.eps}\end{figure}$	Figure 7: The background-subtracted PN count rate in the energy band MHX (700 to 12 000 eV) ( top 2005/03/31, bottom 2006/04/06) binned to 30 s, plotted over spin-phase ( upper). The same data, binned into 50 phase bins with an overplotted spline fit ( lower).
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$\begin{figure} \par\includegraphics[height=13.57cm,angle=0,clip]{7013_fig9.eps}\end{figure}$	Figure 9: Light curves in the hard and soft X-ray bands from 2005 folded on the period corresponding to $\omega -\Omega /2$ (error bars in the light curves are the standard deviation of the values having entered the bin), and the free parameters of the fits to the phase-resolved spectra.
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$\begin{figure} \par\includegraphics[height=13.5cm,angle=0,clip]{7013_fig10.eps}\end{figure}$	Figure 10: The orbital period $\Omega$ : light curves from 2005 in the hard and soft X-ray bands, the fitted spectral parameters, and the phase-folded R-band data. The error bars of the light curves are the standard deviation of the values having entered the bin.
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