All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4460F1.eps}\end{figure}$ Figure 1: Upper panel: phase-folded diagram of the radial velocities of HD 192263. The solid curve represents the best Keplerian fit. Middle panel: periodogram of the radial velocities, showing a very well defined peak at the observed $\sim$ 24.4-day period. Lower panel: residuals of the 24.4-day orbital solution, showing the presence of a long term trend in the data. The line represents a linear fit, and has a slope of 4.8 $~\pm~$ 0.8 m s^-1 yr^-1.
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In the text

$\begin{figure} \par\includegraphics[width=15.6cm,clip]{H4460F2.eps}\end{figure}$ Figure 2: Radial-velocity time series of HD 192263 for the complete span of our measurements. The curve represents the fitted orbital solution.It is interesting to see the long-term phase stability of the radial-velocity signal.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4460F3.eps}\end{figure}$ Figure 3: Upper panel: radial velocity vs. BIS for HD 192263 (as defined in Queloz et al. 2001). The slope and its uncertainty are indicated. The Spearman correlation coefficient between the two variables is 0.18. Middle panel: BIS values phase folded with the orbital period. Lower panel: FT of the BIS values. No significant period is found in the data. The dotted line is positioned at the period of 24.4-days. Only the best measurements (with errors lower than 10 m s^-1) are considered in these three plots.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{H4460F4.eps}\end{figure}$ Figure 4: Upper panels: modeled amplitudes of bisector inverse slope (BIS) and radial velocity, induced by spots with filling factors of 5% and 1% (solid and dotted line, respectively), plotted as a function of the star's projected rotational velocity. Lower panel: amplitude ratios (in percent) as a function of $v~\sin{i}$ . These results were obtained with a very simple model, and should be considered only as qualitative. See text for more details.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{H4460F5.eps}\end{figure}$ Figure 5: Photometric measurements of Henry et al. (2002) plotted as a function of time. The three panels correspond to panels 4, 5 and 6 of Fig. 2. Superimposed with the photometry is a sinusoidal curve with the same period and phase as the radial-velocity Keplerian fit.
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In the text

$\begin{figure} \par\includegraphics[width=8.35cm,clip]{H4460F6.eps}\end{figure}$ Figure 6: Plots of the GENEVA-photometry points (upper panel) and 3-day binned photometric data (second panel, solid line), CORALIE radial velocities, residuals to the Keplerian fit (OCFT), and BIS values, as a function of time for the period of simultaneous observations. The sinusoidal curve on top of the velocity points (third panel) illustrates the global Keplerian solution obtained for our data (see Sect. 3). For the two panels with the photometric data, the "fitted'' dotted line has the same period and phase as for the radial velocities.
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In the text

$\begin{figure} \par\includegraphics[width=15.6cm,clip]{H4460F2.eps}\end{figure}$	Figure 2: Radial-velocity time series of HD 192263 for the complete span of our measurements. The curve represents the fitted orbital solution.It is interesting to see the long-term phase stability of the radial-velocity signal.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{H4460F5.eps}\end{figure}$	Figure 5: Photometric measurements of Henry et al. (2002) plotted as a function of time. The three panels correspond to panels 4, 5 and 6 of Fig. 2. Superimposed with the photometry is a sinusoidal curve with the same period and phase as the radial-velocity Keplerian fit.
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