All Figures

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2826fig1.ps} \end{figure}$ Figure 1: The HARPS spectrum of the three stars HD 2638, HD 27894, and HD 63454 around the CaII H absorption line. The emission peak in the core of the absorption band is significant for HD 63454 but still shows a fair level of activity.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2826fig2.ps} \end{figure}$ Figure 2: The stars HD 2638, HD 27894, and HD 63454 over the evolutionary tracks calculated for 0.7, 0.8, and 0.9 $M_{\odot }$ metal-rich stars (Baraffe et al. 1998). The dashed lines are comparison tracks for solar-metallicity stars.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2826fig3.ps} \end{figure}$ Figure 3: The radial-velocity curve of HD 2638 obtained with HARPS. Top: with phase-folding; Bottom: individual radial-velocity measurements versus time.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2826fig4.ps} \end{figure}$ Figure 4: The inverse bisector slope plotted against the radial velocity of HD 2638 ( top) and against the planet phase ( bottom). No correlation between these quantities is observed.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2826fig5.ps} \end{figure}$ Figure 5: The HARPS radial-velocity curve of HD 27894.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2826fig6.ps} \end{figure}$ Figure 6: The inverse bisector slope is plotted against the radial velocity of HD 27894 ( top) and against the planet phase ( bottom). No correlation between these quantities is observed.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2826fig7.ps} \end{figure}$ Figure 7: The radial-velocity curve of HD 63454. Open circles show CORALIE data, while filled circles show HARPS data.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2826fig8.ps} \end{figure}$ Figure 8: The inverse bisector slope is plotted against the radial velocity of HD 63454 ( top) and against the planet phase ( bottom). No correlation between these quantities is observed.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2826fig9.ps} \end{figure}$ Figure 9: The mass period diagram for all known short-period planets. Open circles stand for planets orbiting subsolar-metallicity stars while filled circles correspond to planets around metal-rich stars. Squares indicate those planets with unmeasured metallicity. The dark-filled circles show the lower-mass, possibly rocky planets. The three planets described in this paper are marked with a lozenge. The vast majority of planet-bearing stars are metal-rich in this corner of the (M, P) diagram, and the new HARPS planets support this observation.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2826fig1.ps} \end{figure}$	Figure 1: The HARPS spectrum of the three stars HD 2638, HD 27894, and HD 63454 around the CaII H absorption line. The emission peak in the core of the absorption band is significant for HD 63454 but still shows a fair level of activity.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{2826fig2.ps} \end{figure}$	Figure 2: The stars HD 2638, HD 27894, and HD 63454 over the evolutionary tracks calculated for 0.7, 0.8, and 0.9 $M_{\odot }$ metal-rich stars (Baraffe et al. 1998). The dashed lines are comparison tracks for solar-metallicity stars.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2826fig3.ps} \end{figure}$	Figure 3: The radial-velocity curve of HD 2638 obtained with HARPS. Top: with phase-folding; Bottom: individual radial-velocity measurements versus time.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2826fig4.ps} \end{figure}$	Figure 4: The inverse bisector slope plotted against the radial velocity of HD 2638 ( top) and against the planet phase ( bottom). No correlation between these quantities is observed.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2826fig5.ps} \end{figure}$	Figure 5: The HARPS radial-velocity curve of HD 27894.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2826fig6.ps} \end{figure}$	Figure 6: The inverse bisector slope is plotted against the radial velocity of HD 27894 ( top) and against the planet phase ( bottom). No correlation between these quantities is observed.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2826fig7.ps} \end{figure}$	Figure 7: The radial-velocity curve of HD 63454. Open circles show CORALIE data, while filled circles show HARPS data.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2826fig8.ps} \end{figure}$	Figure 8: The inverse bisector slope is plotted against the radial velocity of HD 63454 ( top) and against the planet phase ( bottom). No correlation between these quantities is observed.
Open with DEXTER