$\begin{figure} \par\includegraphics[height=9cm,angle=90,clip]{7683fig1a.ps}\includegraphics[height=9cm,angle=90,clip]{7683fig1b.ps}\end{figure}$ Figure 1: Left: time/frequency diagramme of Procyon data, showing excess power between 500 and 1200 $\mu$ Hz during the first eight days of observation. Right: same analysis of the CCD temperature, showing the same excess of power.
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In the text

$\begin{figure} \par\includegraphics[height=8.5cm,angle=90,clip]{7683fig2.ps}\end{figure}$ Figure 2: Time variation of the integrated power (from 400 to 1600 $\mu$ Hz), showing two different levels during the observations.
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In the text

$\begin{figure} \par\includegraphics[height=8.5cm,angle=90,clip]{7683fig3.ps}\end{figure}$ Figure 3: Smoothed Fourier spectra of Procyon data for the first seven days (black) and last 25 days (grey) of observation.
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In the text

$\begin{figure} \par\includegraphics[height=9cm,angle=90,clip]{7683fig4.ps}\end{figure}$ Figure 4: Collapsed echelle diagramme for simulated data, showing the signature of regular spacing of $\simeq$ 82 $\mu$ Hz and multiples of this spacing as defined in Eq. (4).
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In the text

$\begin{figure} \par\includegraphics[height=9cm,angle=90,clip]{7683fig5.ps}\end{figure}$ Figure 5: Power spectrum of the window function of the observation, almost perfect but presenting some weak but regularly-spaced peaks.
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In the text

$\begin{figure} \par\includegraphics[height=8.5cm,angle=90,clip]{7683fig6a.ps}\includegraphics[height=8.5cm,angle=90]{7683fig6b.ps}\end{figure}$ Figure 6: Left: collapsed echelle diagramme for the Procyon window function. It is dominated by a peak at $\simeq$ 165 $\mu$ Hz corresponding to the orbital frequency, and other peaks following Eq. (4). Right: same diagramme for Procyon data, with similar patterns.
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In the text

$\begin{figure} \par\includegraphics[height=9cm,angle=90,clip]{7683fig1a.ps}\includegraphics[height=9cm,angle=90,clip]{7683fig1b.ps}\end{figure}$	Figure 1: Left: time/frequency diagramme of Procyon data, showing excess power between 500 and 1200 $\mu$ Hz during the first eight days of observation. Right: same analysis of the CCD temperature, showing the same excess of power.
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$\begin{figure} \par\includegraphics[height=8.5cm,angle=90,clip]{7683fig2.ps}\end{figure}$	Figure 2: Time variation of the integrated power (from 400 to 1600 $\mu$ Hz), showing two different levels during the observations.
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$\begin{figure} \par\includegraphics[height=8.5cm,angle=90,clip]{7683fig3.ps}\end{figure}$	Figure 3: Smoothed Fourier spectra of Procyon data for the first seven days (black) and last 25 days (grey) of observation.
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$\begin{figure} \par\includegraphics[height=9cm,angle=90,clip]{7683fig4.ps}\end{figure}$	Figure 4: Collapsed echelle diagramme for simulated data, showing the signature of regular spacing of $\simeq$ 82 $\mu$ Hz and multiples of this spacing as defined in Eq. (4).
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$\begin{figure} \par\includegraphics[height=9cm,angle=90,clip]{7683fig5.ps}\end{figure}$	Figure 5: Power spectrum of the window function of the observation, almost perfect but presenting some weak but regularly-spaced peaks.
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$\begin{figure} \par\includegraphics[height=8.5cm,angle=90,clip]{7683fig6a.ps}\includegraphics[height=8.5cm,angle=90]{7683fig6b.ps}\end{figure}$	Figure 6: Left: collapsed echelle diagramme for the Procyon window function. It is dominated by a peak at $\simeq$ 165 $\mu$ Hz corresponding to the orbital frequency, and other peaks following Eq. (4). Right: same diagramme for Procyon data, with similar patterns.
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$\begin{figure} \par\includegraphics[height=8.5cm,angle=90,clip]{7683fig7a.ps}\includegraphics[height=8.5cm,angle=90]{7683fig7b.ps}\end{figure}$	Figure 7: Respective enlargements of the Fig. 6. The discontinuous appearance is due do the discrete frequency sampling of the spectra.
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