All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4076_f1.eps} \end{figure}$ Figure 1: ELODIE data. Top: $RV-\langle RV\rangle$ for GJ 777 A. Bottom: residuals of HD 71148, a radial-velocity constant G5V star. The residuals slope is compatible with zero whereas a clear trend is seen for GJ 777 A. This demonstrates that the GJ 777 A radial-velocity signal does not result from some undesirable instrumental effect.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4076_f2.eps} \end{figure}$ Figure 2: Top: ELODIE (filled circles) and AFOE (open circles) temporal velocities. The fitted eccentric orbit is shown (solid line). The radial-velocity maximum is not well covered. This probably tends to artificially increase the fitted eccentricity. The fitted circular orbit (dotted line) is also plotted for comparison. Bottom: residuals to the fitted eccentric orbit.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4076_f1.eps} \end{figure}$	Figure 1: ELODIE data. Top: $RV-\langle RV\rangle$ for GJ 777 A. Bottom: residuals of HD 71148, a radial-velocity constant G5V star. The residuals slope is compatible with zero whereas a clear trend is seen for GJ 777 A. This demonstrates that the GJ 777 A radial-velocity signal does not result from some undesirable instrumental effect.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4076_f2.eps} \end{figure}$	Figure 2: Top: ELODIE (filled circles) and AFOE (open circles) temporal velocities. The fitted eccentric orbit is shown (solid line). The radial-velocity maximum is not well covered. This probably tends to artificially increase the fitted eccentricity. The fitted circular orbit (dotted line) is also plotted for comparison. Bottom: residuals to the fitted eccentric orbit.
Open with DEXTER