All Figures

$\begin{figure} \par\includegraphics[height=7.9cm,width=7.65cm,clip]{3877fig1.ps}\end{figure}$ Figure 1: The grand average optical spectrum of RX J1548.
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In the text

$\begin{figure} \par\includegraphics[height=8.5cm,width=7.55cm,clip]{3877fig2a.ps... ...*{8mm} \includegraphics[height=8.5cm,width=7.3cm,clip]{3877fig2b.ps}\end{figure}$ Figure 2: Enlargements around the orbital ( left) and the spin ( right) frequencies of the DFTs of radial velocities of emission lines (Balmer, He II and He I) and their CLEANED power spectra (at their right side). Vertical dotted lines from left to right mark the positions of the orbital, beat and spin frequencies.
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In the text

$\begin{figure} \par\includegraphics[height=8.5cm,width=7.65cm,clip]{3877fig3a.ps... ...{7mm} \includegraphics[height=8.5cm,width=7.35cm,clip]{3877fig3b.ps}\end{figure}$ Figure 3: Enlargements around the orbital ( left) and the spin ( right) frequencies of the DFTs of EWs of emission lines (Balmer, He II and He I) and their CLEANED power spectra (at their right side). The positions of the orbital, its first harmonic, the beat and spin frequencies are also marked with vertical dotted lines.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{3877fig4.ps}\end{figure}$ Figure 4: Upper panel: the continuum flux light curve measured in line-free regions of the spectrum from 4040 to 6800 $\AA$ . Lower panel: The DFT of the continuum light curve. Middle panel: the CLEANED power spectrum of the same time series. Note the absence of signal at the spin and beat frequency and the presence of power at the orbital frequency. The spectral window of the data is shown in the inserted panel. The peaks at $\sim$ 20 day^-1, partially due to the spectral window and hence partially removed by the CLEAN algorithm, are likely due to slit losses (see text).
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In the text

$\begin{figure} \par\includegraphics[height=12cm,width=8cm,clip]{3877fig5a.ps}\includegraphics[height=12cm,width=8cm,clip]{3877fig5b.ps}\end{figure}$ Figure 5: Left: the radial velocity curves of Balmer emissions and He II $\lambda$ 4686 and He I $\lambda$ 5875 together with their best fit two-sine function at the spin and orbital periods. Note the excursion at the beginning of the second night observed in the blue spectra. The arrow marks the H $_{\alpha }$ radial velocity measurement on the red spectrum acquired just after the first sequence of blue spectra (see text). Center: the folded spin radial velocity curves of the same emission lines in 20 phase bins detrended from the orbital modulation together with their best fit sinusoidal function. Right: folded orbital radial velocity curves in 20 phase bins detrended from the rotational variability together with their best sine fit. The radial velocities of the absorption components in Balmer lines as measured on the 10 binned phase folded spectra at the spin and orbital periods are also reported with open squares and also showing larger error bars. No orbital modulation could be measured in the absorption of H $_{\delta }$ line (see text). $\gamma$ velocities have been subtracted.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.25cm,clip]{3877fig6.ps}\end{figure}$ Figure 6: The $\chi ^2$ periodogram of the radial velocities of emission lines of H $_{\alpha }$ (filled squares), H $_{\beta }$ (open squares), H $_{\gamma }$ (open diamonds), H $_{\delta }$ (diagonal crosses), He I (crosses) and He II (open triangles). The best value is found for H $_{\alpha }$ line.
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In the text

$\begin{figure} \par\includegraphics[width=6.65cm,clip]{3877fig7.ps}\end{figure}$ Figure 7: Radial velocity curves obtained from cross-correlation of emission and telluric line free portion of the spectrum of RX J1548 with a set of late type template star spectra.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3877fig8.ps}\end{figure}$ Figure 8: The WD (thick curves) and secondary star (thin curves) masses versus inclination adopting a mass ratio q=0.65 $\pm$ 0.12. The dashed upper and lower curves correspond to the uncertainties in the mass ratio. The lower limit on inclination is set by the Chandrasekhar limit for the WD mass. The main sequence mass-spectral type relation is also reported on the right side. Horizontal dotted lines mark the adopted range of spectral types for the secondary star.
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In the text

$\begin{figure} \par\includegraphics[height=7.9cm,width=7.65cm,clip]{3877fig1.ps}\end{figure}$	Figure 1: The grand average optical spectrum of RX J1548.
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$\begin{figure} \par\includegraphics[height=8.5cm,width=7.55cm,clip]{3877fig2a.ps... ...*{8mm} \includegraphics[height=8.5cm,width=7.3cm,clip]{3877fig2b.ps}\end{figure}$	Figure 2: Enlargements around the orbital ( left) and the spin ( right) frequencies of the DFTs of radial velocities of emission lines (Balmer, He II and He I) and their CLEANED power spectra (at their right side). Vertical dotted lines from left to right mark the positions of the orbital, beat and spin frequencies.
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$\begin{figure} \par\includegraphics[height=8.5cm,width=7.65cm,clip]{3877fig3a.ps... ...{7mm} \includegraphics[height=8.5cm,width=7.35cm,clip]{3877fig3b.ps}\end{figure}$	Figure 3: Enlargements around the orbital ( left) and the spin ( right) frequencies of the DFTs of EWs of emission lines (Balmer, He II and He I) and their CLEANED power spectra (at their right side). The positions of the orbital, its first harmonic, the beat and spin frequencies are also marked with vertical dotted lines.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.25cm,clip]{3877fig6.ps}\end{figure}$	Figure 6: The $\chi ^2$ periodogram of the radial velocities of emission lines of H $_{\alpha }$ (filled squares), H $_{\beta }$ (open squares), H $_{\gamma }$ (open diamonds), H $_{\delta }$ (diagonal crosses), He I (crosses) and He II (open triangles). The best value is found for H $_{\alpha }$ line.
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$\begin{figure} \par\includegraphics[width=6.65cm,clip]{3877fig7.ps}\end{figure}$	Figure 7: Radial velocity curves obtained from cross-correlation of emission and telluric line free portion of the spectrum of RX J1548 with a set of late type template star spectra.
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