All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{7361fig1.eps} \end{figure}$ Figure 1: Top: HARPS radial-velocity data (dots) for HD 100777 and fitted orbital solution (solid curve). The radial-velocity signal is induced by the presence of a 1.16 $M_{\rm Jup}$ planetary companion on a 384-day orbit. Bottom: residuals to the fitted orbit. The scatter of these residuals is compatible with the velocity uncertainties.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7361fig2.eps} \end{figure}$ Figure 2: Top: HARPS radial-velocity data (dots) for HD 190647 and fitted orbital solution (solid curve). The radial-velocity signal is induced by the presence of a 1.9 $M_{\rm Jup}$ planetary companion on a 1038-day orbit. Bottom: residuals to the fitted orbit. The scatter of these residuals is compatible with the velocity uncertainties.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7361fig3.eps} \end{figure}$ Figure 3: Top: HARPS radial-velocity data (dots) for HD 221287 and fitted orbital solution (solid curve). The detected Keplerian signal is induced by a 3.1 $M_{\rm Jup}$ planet on a 456-day orbit. Because of a non-optimal coverage of the radial-velocity maximum and the presence of stellar activity-induced jitter, the exact shape of the orbit is not very well-constrained. Bottom: residuals to the fitted orbit. The scatter of these residuals is much larger than the velocity uncertainties. This large dispersion is probably due to the fairly high activity level of this star.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7361fig4.eps} \end{figure}$ Figure 4: a) Bisector span versus radial-velocity plot for HD 221287. The dispersion of the span data is quite large (10.4 m s $^{\rm -1}$ ) revealing potential line-profile variations. Nevertheless, the main radial-velocity signal is not correlated to these profile variations and is thus certainly of Keplerian origin. b) Bisector span versus radial-velocity residuals to the Keplerian orbit (see Table 5) displayed in the same velocity scale. A marginal anti-correlation between the two quantities is observed.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7361fig1.eps} \end{figure}$	Figure 1: Top: HARPS radial-velocity data (dots) for HD 100777 and fitted orbital solution (solid curve). The radial-velocity signal is induced by the presence of a 1.16 $M_{\rm Jup}$ planetary companion on a 384-day orbit. Bottom: residuals to the fitted orbit. The scatter of these residuals is compatible with the velocity uncertainties.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{7361fig2.eps} \end{figure}$	Figure 2: Top: HARPS radial-velocity data (dots) for HD 190647 and fitted orbital solution (solid curve). The radial-velocity signal is induced by the presence of a 1.9 $M_{\rm Jup}$ planetary companion on a 1038-day orbit. Bottom: residuals to the fitted orbit. The scatter of these residuals is compatible with the velocity uncertainties.
Open with DEXTER