All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.9cm,clip]{9341fig1.ps}\end{figure}$ Figure 1: Combined PN and MOS light curve with a binning of 110 s for the energy range 0.15-12.0 keV. Zeropoint is BJD = 2 453 185.0. For a phase folded light curve see Fig. 5.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9341fig2.ps}\end{figure}$ Figure 2: Finding chart of 2XMM1312 created with the SDSS finding chart tool. The new CV, the nearby AGN and the comparison star used for differential photometry are marked.
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In the text

$\begin{figure} \par\includegraphics[width=8.9cm,clip]{9341fig3.ps}\end{figure}$ Figure 3: Average spectrum of 2XMM1312 (=SDSS J131223.48+ 173659.1) obtained on February 16, 2007, with the CA 2.2 m telescope and CAFOS (total exposure 100 min).
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In the text

$\begin{figure} \par\includegraphics[width=8.9cm,clip]{9341fig4.ps}\end{figure}$ Figure 4: Average spectrum of the quasar SDSS J131223.75+173701.2 obtained on February 16, 2007.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{9341fig5.ps}\end{figure}$ Figure 5: The upper panel shows the phase folded X-ray light curve from 2004 composed of EPIC PN and MOS counts with a binning of 0.02 phase units. The lower panel shows the phase folded R band light curve from March 2007.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{9341fig6.ps}\vspace*{2mm} \includegraphics[angle=-90,width=8.8cm,clip]{9341fig7.ps}\end{figure}$ Figure 6: Spectral fit of the combined PN and MOS mean spectra with an absorbed MEKAL model, together with the confidence range (0.68, 0.90 and 0.99) as a function of the MEKAL temperature and the column density of the interstellar absorption.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{9341fig8.ps}\vspace*{1mm} \includegraphics[angle=-90,width=8.7cm,clip]{9341fig9.ps}\end{figure}$ Figure 7: Spectral fit of the combined PN and MOS spectra of the X-ray bright phase before the absorption dip with an absorbed MEKAL model, together with the confidence range (0.68, 0.90 and 0.99) as a function of the MEKAL temperature and the column density of the interstellar absorption. The bright phase interval was selected individually for each of the five orbits. Note the different scaling of the y axis compared to Fig. 6.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{9341fig10.ps}\end{figure}$ Figure 8: Optical light curves in BVR (in descending order for the upper plot and ascending order for the lower plot) bandpasses determined from flux-calibrated phase-resolved spectra of February 16, 2007. We estimated the errors from our reduction procedure to $\sim$ 0.12 $.\!\!^{\rm m}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{9341fig11.ps}\end{figure}$ Figure 9: Spectral energy distribution with all available data: 2MASS upper limits (arrows on the left), CAHA mean spectrum (next to the arrows), XMM OM (next to the long dashed line) and XMM EPIC spectrum (on the right). Overplotted (long dash) is a 10 eV black body providing a negligible fraction of 10% of the observed soft X-ray flux (see Sect. 3.2 for a discussion of this component) and the MEKAL model spectrum (dotted line).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{9341fig12.ps}\end{figure}$ Figure 10: PN light curve for soft (0.15-1.25 keV) and hard (1.25-12.0 keV) energy ranges together with the resulting hardness ratio. Soft and hard band contain approximately an equal number of photons ( $\sim$ 3100).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{9341fig13.ps}\end{figure}$ Figure 11: Spectral fit of the combined PN and MOS spectra for the phase intervals of the absorption dip (visually selected for each orbit) with an absorbed MEKAL model. Plasma temperature and normalisation were fixed to the fitting values of the bright phase spectrum before the absorption dip.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.9cm,clip]{9341fig14.ps}\end{figure}$ Figure 12: Mean eclipse light curve from the optical R band observations on March 19 (errors are smaller than symbol size). Ingress and egress of accretion spot and accretion stream are clearly identifiable. Non-detections are set to zero.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.9cm,clip]{9341fig1.ps}\end{figure}$	Figure 1: Combined PN and MOS light curve with a binning of 110 s for the energy range 0.15-12.0 keV. Zeropoint is BJD = 2 453 185.0. For a phase folded light curve see Fig. 5.
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$\begin{figure} \par\includegraphics[width=9cm,clip]{9341fig2.ps}\end{figure}$	Figure 2: Finding chart of 2XMM1312 created with the SDSS finding chart tool. The new CV, the nearby AGN and the comparison star used for differential photometry are marked.
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$\begin{figure} \par\includegraphics[width=8.9cm,clip]{9341fig3.ps}\end{figure}$	Figure 3: Average spectrum of 2XMM1312 (=SDSS J131223.48+ 173659.1) obtained on February 16, 2007, with the CA 2.2 m telescope and CAFOS (total exposure 100 min).
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$\begin{figure} \par\includegraphics[width=8.9cm,clip]{9341fig4.ps}\end{figure}$	Figure 4: Average spectrum of the quasar SDSS J131223.75+173701.2 obtained on February 16, 2007.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{9341fig5.ps}\end{figure}$	Figure 5: The upper panel shows the phase folded X-ray light curve from 2004 composed of EPIC PN and MOS counts with a binning of 0.02 phase units. The lower panel shows the phase folded R band light curve from March 2007.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm,clip]{9341fig6.ps}\vspace*{2mm} \includegraphics[angle=-90,width=8.8cm,clip]{9341fig7.ps}\end{figure}$	Figure 6: Spectral fit of the combined PN and MOS mean spectra with an absorbed MEKAL model, together with the confidence range (0.68, 0.90 and 0.99) as a function of the MEKAL temperature and the column density of the interstellar absorption.
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$\begin{figure} \par\includegraphics[width=8.7cm,clip]{9341fig10.ps}\end{figure}$	Figure 8: Optical light curves in BVR (in descending order for the upper plot and ascending order for the lower plot) bandpasses determined from flux-calibrated phase-resolved spectra of February 16, 2007. We estimated the errors from our reduction procedure to $\sim$ 0.12 $.\!\!^{\rm m}$ .
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{9341fig12.ps}\end{figure}$	Figure 10: PN light curve for soft (0.15-1.25 keV) and hard (1.25-12.0 keV) energy ranges together with the resulting hardness ratio. Soft and hard band contain approximately an equal number of photons ( $\sim$ 3100).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{9341fig13.ps}\end{figure}$	Figure 11: Spectral fit of the combined PN and MOS spectra for the phase intervals of the absorption dip (visually selected for each orbit) with an absorbed MEKAL model. Plasma temperature and normalisation were fixed to the fitting values of the bright phase spectrum before the absorption dip.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.9cm,clip]{9341fig14.ps}\end{figure}$	Figure 12: Mean eclipse light curve from the optical R band observations on March 19 (errors are smaller than symbol size). Ingress and egress of accretion spot and accretion stream are clearly identifiable. Non-detections are set to zero.
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