All Figures

$\begin{figure} \par\mbox{\fbox{ \includegraphics[width=70mm]{7684fig1.ps}}\fbox{ \par \includegraphics[width=70mm]{7684fig2.ps}} }\end{figure}$ Figure 1: Left: ROSAT X-ray image of RX J0524+42 including the SNR that inspired its name, Paloma. The field of view is about $60\hbox {$^\prime $ }\times 60\hbox {$^\prime $ }$ and the CV is the bright point source $\sim$ $15\hbox {$^\prime $ }$ west of the SNR. Right: V-band CCD image of Paloma obtained with the AIP 70 cm telescope. North is on top and east to the left. The size of the field is approximately $5\hbox {$^\prime $ }\times 5 \hbox {$^\prime $ }$ . The circle refers to the 2 $\sigma$ X-ray positional error. The position of the optical counterpart is $\alpha_{2000} = 05^{\rm h}24^{\rm m}30\hbox{$.\!\!^{\rm s}$ }4$ and $\delta _{2000}=42\hbox {$^\circ $ }44\hbox {$^\prime $ }51\hbox {$^{\prime \prime }$ }$ .
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In the text

$\begin{figure} \par\includegraphics[clip=,angle=-90,width=8.8cm]{7684fig3.ps} \end{figure}$ Figure 2: Average low-resolution spectrum of Paloma derived from a series of 32 exposures taken on November 2, 1995. The flux scale has been calibrated to match the brightness level of the photometric observation on November 24, 1995. What appears as sharp absortions features are detector artefacts.
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In the text

$\begin{figure} \par\includegraphics[clip=,angle=-90,width=8.8cm]{7684fig4.ps} \end{figure}$ Figure 3: Long-term light curve of Paloma.
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In the text

$\begin{figure} \center{\includegraphics[clip=,width=8cm]{7684fig5.ps} }\end{figure}$ Figure 4: Example light curves of Paloma.
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In the text

$\begin{figure} \center{ \includegraphics[clip=,angle=-90,width=17cm]{7684fig6.ps} }\end{figure}$ Figure 5: AoV-periodogram of Paloma computed for photometric data obtained from 1998 to 2002. The fundamental periods P₁, P₂, and P₃ and their most obvious aliases are marked. In this paper P₁ at 157 min is adopted as the orbital period, while the white dwarf spin can be alternatively associated with P₂ (case A) or P₃ (case B). The third periodicity is a composite of orbital and spin period and either corresponds to the $2\omega -\Omega$ frequency (as P₃ = 136 min - case A) or to the sub-harmonic of the side-band frequency $(\omega +\Omega )/2$ (as P₂ = 147 min - case B).
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In the text

$\begin{figure} \par\includegraphics[clip=,angle=-90,width=8.8cm]{7684fig7.ps} \end{figure}$ Figure 6: Detailed view of the AoV periodogram around the three main signals.
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In the text

$\begin{figure} \par\includegraphics[clip=,angle=0,width=8.8cm]{7684fig8.ps} \end{figure}$ Figure 7: AoV-periodogram of Paloma in the low frequency range showing a strong signal at 1.41915 days close to, but not exactly at the expected beat period of 1.42205 days.
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In the text

$\begin{figure} \center{\includegraphics[clip=,width=18cm]{7684fig9.ps} }\end{figure}$ Figure 8: Collection of all optical data taken in January 2002 folded over the beat period of 1.4 days (case A). Small numbers denote the day of month. In the lower panel the above data are phase-averaged.
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In the text

$\begin{figure} \par\includegraphics[clip=,width=17cm]{7684fig10.ps} \end{figure}$ Figure 9: Optical light curves from January 2002 as a function of spin phase separated into 14 individual sections of the 1.4 day beat period.
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In the text

$\begin{figure} \par\includegraphics[clip=,width=8.5cm]{7684fig11.ps} \end{figure}$ Figure 10: Spin folded light curves from January 2002 data of Paloma now assuming P₃ = 136 min as the true spin period (case B). The data are split into 7 individual sections of the beat cycle of 0.7 days.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{7684fig12.ps} \end{figure}$ Figure 11: X-ray light curves of Paloma from the two ROSAT PSPC pointings. The data is phased according to the spin period P₂ (case A). The longer PSPC pointing have been splitted into two sections of different beat phase intervals.
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In the text

$\begin{figure} \par\center{\includegraphics[clip=,angle=-90,width=17cm]{7684fig13.ps} }\end{figure}$ Figure 12: The degree of asynchronism ( $(P_{\rm orb}-P_{\rm spin})/P_{\rm orb}\times 100\%)$ of magnetic CVs as a function of orbital period. The different subtypes are denoted by: DQ Herculis stars (open circles), AM Herculis stars (filled circles), and the four near-synchronous polars (crosses).
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In the text

$\begin{figure} \par\includegraphics[clip=,angle=-90,width=8.8cm]{7684fig3.ps} \end{figure}$	Figure 2: Average low-resolution spectrum of Paloma derived from a series of 32 exposures taken on November 2, 1995. The flux scale has been calibrated to match the brightness level of the photometric observation on November 24, 1995. What appears as sharp absortions features are detector artefacts.
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$\begin{figure} \par\includegraphics[clip=,angle=-90,width=8.8cm]{7684fig4.ps} \end{figure}$	Figure 3: Long-term light curve of Paloma.
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$\begin{figure} \center{\includegraphics[clip=,width=8cm]{7684fig5.ps} }\end{figure}$	Figure 4: Example light curves of Paloma.
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$\begin{figure} \par\includegraphics[clip=,angle=-90,width=8.8cm]{7684fig7.ps} \end{figure}$	Figure 6: Detailed view of the AoV periodogram around the three main signals.
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$\begin{figure} \par\includegraphics[clip=,angle=0,width=8.8cm]{7684fig8.ps} \end{figure}$	Figure 7: AoV-periodogram of Paloma in the low frequency range showing a strong signal at 1.41915 days close to, but not exactly at the expected beat period of 1.42205 days.
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$\begin{figure} \center{\includegraphics[clip=,width=18cm]{7684fig9.ps} }\end{figure}$	Figure 8: Collection of all optical data taken in January 2002 folded over the beat period of 1.4 days (case A). Small numbers denote the day of month. In the lower panel the above data are phase-averaged.
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$\begin{figure} \par\includegraphics[clip=,width=17cm]{7684fig10.ps} \end{figure}$	Figure 9: Optical light curves from January 2002 as a function of spin phase separated into 14 individual sections of the 1.4 day beat period.
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$\begin{figure} \par\includegraphics[clip=,width=8.5cm]{7684fig11.ps} \end{figure}$	Figure 10: Spin folded light curves from January 2002 data of Paloma now assuming P₃ = 136 min as the true spin period (case B). The data are split into 7 individual sections of the beat cycle of 0.7 days.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{7684fig12.ps} \end{figure}$	Figure 11: X-ray light curves of Paloma from the two ROSAT PSPC pointings. The data is phased according to the spin period P₂ (case A). The longer PSPC pointing have been splitted into two sections of different beat phase intervals.
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$\begin{figure} \par\center{\includegraphics[clip=,angle=-90,width=17cm]{7684fig13.ps} }\end{figure}$	Figure 12: The degree of asynchronism ( $(P_{\rm orb}-P_{\rm spin})/P_{\rm orb}\times 100\%)$ of magnetic CVs as a function of orbital period. The different subtypes are denoted by: DQ Herculis stars (open circles), AM Herculis stars (filled circles), and the four near-synchronous polars (crosses).
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