All Figures

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0574_f1.eps}\end{figure}$ Figure 1: Doppler shift measurements over seven nights from two-sites observations of Procyon A (black dots: ELODIE data, green dots: AFOE data).
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0574_f2.eps}\end{figure}$ Figure 2: Power spectrum of Procyon A from Doppler shift measurements over 15 h, with ELODIE and AFOE.
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In the text

$\begin{figure} \par\mbox{\hspace*{3.2cm}\footnotesize ELODIE 1999\hspace*{7.3cm}... ...ics{0574_f3c.eps}}\scalebox{0.50}{\includegraphics{0574_f3d.eps}} } \end{figure}$ Figure 3: Top panels: power spectra of the ELODIE and AFOE Doppler shift measurements (7 nights) of Procyon. Bottom left panel: power spectrum of the combined data sets. Bottom right panel: simulated spectrum computed with noise and with the same observation times as the combined sequence ELODIE/AFOE.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0574_f4.eps}\end{figure}$ Figure 4: Comparison between modified comb responses computed for two central frequencies of the power spectrum of Procyon data (see description in text).
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In the text

$\begin{figure} \par\scalebox{0.5}{\includegraphics[clip]{0574_f5a.eps}}\vspace{0.1cm} \par\scalebox{0.5}{\includegraphics[clip]{0574_f5b.eps}}\par\end{figure}$ Figure 5: Top panel: the first-order spacings over several frequency ranges, as determined from comb analysis. Bottom panel: echelle diagram of the selected frequencies with the best comb responses (l=0, 1 indicated respectively by diamonds and triangles).
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{0574_f6.eps}\end{figure}$ Figure 6: Example of an echelle diagram from Procyon amplitude spectrum of the joint ELODIE and AFOE radial velocity measurements, computed for the modulo mean $\Delta \nu _{\rm0}= 54$ $\mu$ Hz. The frequencies from the standard model (see Chaboyer et al. 1999) are indicated by asterisks, plus signs and squares respectively for l=0,1,2, dashed lines are at $l=0,1,2 \pm11.6~\mu$ Hz). The inset shows the colour coding applied to the values in each succesive folding frequency range.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0574_f7.eps} \end{figure}$ Figure 7: Identification of the p-modes in the region of the excess power of Procyon A. Dashed lines in blue, red and green correspond respectively to modes l=2,0,1.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0574_f8.eps} \end{figure}$ Figure 8: Echelle diagram of the identified modes of degrees l=0,1,2 from two-site joint Procyon observations (cf. Table 2). For comparison, we indicate with the symbols in red the frequencies detected from previous OHP/ELODIE 1998 run. Vertical lines correspond to the best fit of the observed frequencies to the asymptotic relation, with $\nu _0=648.4$ $\mu$ Hz, $\Delta\nu_0=53.6~\mu$ Hz and $D_0=0.85~\mu$ Hz.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0574_f9.eps} \end{figure}$ Figure 9: Variation of the large spacing between the modes of same degree, compared to the predicted curve from the standard model for l=0 (Chaboyer et al. 1999). The observed average large separations for l=0,1,2 degree are indicated by the horizontal lines.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0574_f1.eps}\end{figure}$	Figure 1: Doppler shift measurements over seven nights from two-sites observations of Procyon A (black dots: ELODIE data, green dots: AFOE data).
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0574_f2.eps}\end{figure}$	Figure 2: Power spectrum of Procyon A from Doppler shift measurements over 15 h, with ELODIE and AFOE.
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$\begin{figure} \par\mbox{\hspace{3.2cm}\footnotesize ELODIE 1999\hspace{7.3cm}... ...ics{0574_f3c.eps}}\scalebox{0.50}{\includegraphics{0574_f3d.eps}} } \end{figure}$	Figure 3: Top panels: power spectra of the ELODIE and AFOE Doppler shift measurements (7 nights) of Procyon. Bottom left panel: power spectrum of the combined data sets. Bottom right panel: simulated spectrum computed with noise and with the same observation times as the combined sequence ELODIE/AFOE.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0574_f4.eps}\end{figure}$	Figure 4: Comparison between modified comb responses computed for two central frequencies of the power spectrum of Procyon data (see description in text).
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$\begin{figure} \par\scalebox{0.5}{\includegraphics[clip]{0574_f5a.eps}}\vspace{0.1cm} \par\scalebox{0.5}{\includegraphics[clip]{0574_f5b.eps}}\par\end{figure}$	Figure 5: Top panel: the first-order spacings over several frequency ranges, as determined from comb analysis. Bottom panel: echelle diagram of the selected frequencies with the best comb responses (l=0, 1 indicated respectively by diamonds and triangles).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0574_f7.eps} \end{figure}$	Figure 7: Identification of the p-modes in the region of the excess power of Procyon A. Dashed lines in blue, red and green correspond respectively to modes l=2,0,1.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0574_f9.eps} \end{figure}$	Figure 9: Variation of the large spacing between the modes of same degree, compared to the predicted curve from the standard model for l=0 (Chaboyer et al. 1999). The observed average large separations for l=0,1,2 degree are indicated by the horizontal lines.
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