$\begin{figure} \par\includegraphics[width=8.1cm,height=7.8cm,clip]{4079_f04.eps} \end{figure}$ Figure 2: Top: ELODIE radial velocities and orbital solutions for HD 180777. Bottom: residuals to the fitted orbital solution.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=3.4cm,clip]{4079_f05.eps} \inclu... ...]{4079_f07.eps} \includegraphics[width=3.4cm,clip]{4079_f08.eps} } \end{figure}$ Figure 3: Left: cross-correlation functions of HD 180777, before ( top) and after ( bottom) correction from the Keplerian motion. Right: their corresponding summed periodograms (see text), with the same scale in the two cases.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{4079_f09.eps} \end{figure}$ Figure 4: Span of the cross-correlation functions phased with a period of 28.44 days: no periodic variation with this period.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{4079_f10.eps} \end{figure}$ Figure 5: ELODIE radial velocity data for HD 6961, a star constant in radial velocity (dispersion of 63 m s $^{\rm -1}$ ), similar and close to HD 180777. The vertical scale is identical to the one in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{4079_f11.eps} \includegraphi... ...,clip]{4079_f12.eps} \includegraphics[width=5cm,clip]{4079_f13.eps} \end{figure}$ Figure 6: Top: bisectors of the cross-correlation functions of HD 180777; only the bisectors of the spectra giving the largest residuals are represented, in 2 sets. Those corresponding to large positive (resp. negative) residuals have been translated to the left (resp. right), in order to better see the difference between them. Dashed lines represent the median bisectors of the dual set. Center: span of the bisectors as a function of the radial velocity residuals. Bottom: curvatures of the bisectors as a function of the residuals.
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In the text

$\begin{figure} \par\includegraphics[width=5.2cm,clip]{4079_f01.eps} \includegrap... ...lip]{4079_f02.eps} \includegraphics[width=5cm,clip]{4079_f03.eps} \end{figure}$	Figure 1: Radial velocities of HD 180777 obtained with ELODIE ( top), the associated periodogram ( center) and the window function ( bottom).
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$\begin{figure} \par\includegraphics[width=8.1cm,height=7.8cm,clip]{4079_f04.eps} \end{figure}$	Figure 2: Top: ELODIE radial velocities and orbital solutions for HD 180777. Bottom: residuals to the fitted orbital solution.
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$\begin{figure} \par\mbox{\includegraphics[width=3.4cm,clip]{4079_f05.eps} \inclu... ...]{4079_f07.eps} \includegraphics[width=3.4cm,clip]{4079_f08.eps} } \end{figure}$	Figure 3: Left: cross-correlation functions of HD 180777, before ( top) and after ( bottom) correction from the Keplerian motion. Right: their corresponding summed periodograms (see text), with the same scale in the two cases.
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$\begin{figure} \par\includegraphics[width=5cm,clip]{4079_f09.eps} \end{figure}$	Figure 4: Span of the cross-correlation functions phased with a period of 28.44 days: no periodic variation with this period.
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$\begin{figure} \par\includegraphics[width=5cm,clip]{4079_f10.eps} \end{figure}$	Figure 5: ELODIE radial velocity data for HD 6961, a star constant in radial velocity (dispersion of 63 m s $^{\rm -1}$ ), similar and close to HD 180777. The vertical scale is identical to the one in Fig. 1.
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$\begin{figure} \par\includegraphics[width=5cm,clip]{4079_f14.eps} \includegraphi... ...,clip]{4079_f15.eps} \includegraphics[width=5cm,clip]{4079_f16.eps} \end{figure}$	Figure 7: High frequency periodograms of the radial velocities obtainedon HD 180777 ( top) and the phasing of the radial velocities to thecorresponding periods ( bottom).
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