All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2924_f1.eps} \end{figure}$ Figure 1: The Hertzsprung-Russel diagram for the ELODIE main programme sample stars. The six stars with new planet candidates are shown as open triangles. The four curves are the solar metallicity evolutionary tracks for 0.8, 0.9, 1.0 and 1.25 $M_{\hbox {$\odot $ }}$ from Geneva models (Schaller et al. 1992).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2924_f2.eps} \end{figure}$ Figure 2: The histograms of m_V and B-V for the ELODIE main programme sample stars.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2924_f3.eps} \end{figure}$ Figure 3: Histogram of ELODIE radial-velocity weighted rms for constant stars. The 1723 measurements of 111 stars having $P(\chi ^{\rm 2})$ $\geq$ 0.05 and $N_{\rm meas}$ $\geq$ 5 have been used for the plot. These selection criteria are sufficient for eliminating highly active stars but lower activity objects can still be present in the sample. The solid curve represents the distribution of the weighted rms corrected (quadratically) for the photon noise. The main error sources still present in these corrected dispersions are the instrumental error and the stellar jitter. The median of this distribution is 7.8 m s $^{\rm -1}$ and 20% of the stars in this sample have weighted rms lower than 6 m s $^{\rm -1}$ . This latter value is a good estimate of the ELODIE instrumental error. We show for comparison the distribution obtained without correcting for the photon noise (dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2924_f4.eps} \end{figure}$ Figure 4: Radial-velocity measurements in km s $^{\rm -1}$ versus time for four standard stars of the ELODIE programme sample: HD 18803, HD 97711, HD 109358 and HD 117043. The mean photon noise $\langle\epsilon_{\rm pn}\rangle$ is indicated at the lower left of each frame and the measurements photon noise-weighted rms error at the lower right. The time span of these measurements is similar to that for the six stars with planet candidates.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2924_f5.eps} \end{figure}$ Figure 5: The Ca II H line region for the six stars extracted from the co-addition of all spectra available for each star. The 3968.49 Å Ca II H line is indicated by a dotted line. None of the stars exhibits any clear trace of chromospheric emission feature in the line core (see text).
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{2924_f6.eps} \end{figure}$ Figure 6: ELODIE radial-velocity measurements in km s $^{\rm -1}$ versus time for all stars but HD 33636 shown in Fig. 7. Each measurement is plotted with an error bar equal to one estimated standard deviation. The orbital solution resulting from the best Keplerian fit, listed in Table 3 and discussed in the text, is superimposed.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2924_f7.eps} \end{figure}$ Figure 7: ELODIE and CORALIE radial-velocity measurements in km s $^{\rm -1}$ versus time for HD 33636. The 5 CORALIE measurements are indicated by the arrow. Each measurement is plotted with an error bar equal to one estimated standard deviation. Since the computed period is not yet covered, the orbital solution is not displayed for the whole fitted period. The orbital solution resulting from the best Keplerian fit, listed in Table 3 and discussed in the text, is superimposed (solid line). The orbital solution published by Vogt et al. (2002) (dotted line) departs clearly from our solution at the epoch of the most recent measurements.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2924_f8.eps} \end{figure}$ Figure 8: $m_{\rm 2} \sin i$ distribution for the 115 planet candidates discovered so far with $m_{\rm 2} \sin i$ < 18 $M_{\rm Jup}$ . The grey square areas point to the contribution of the additional six new candidates presented in this paper.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{2924_f9.eps} \end{figure}$ Figure 9: The location of the 115 planet candidates discovered so far with $m_{\rm 2} \sin i <18~ M_{\rm Jup}$ in the diagram eccentricity versus period. The six new candidates are shown as open triangles.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2924_fA1.eps} \end{figure}$ Figure A.1: The ELODIE radial-velocity curve for HD 13507 versus time. The fit by the reflex motion due to the companion is superimposed to the measurements.

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2924_f1.eps} \end{figure}$	Figure 1: The Hertzsprung-Russel diagram for the ELODIE main programme sample stars. The six stars with new planet candidates are shown as open triangles. The four curves are the solar metallicity evolutionary tracks for 0.8, 0.9, 1.0 and 1.25 $M_{\hbox {$\odot $ }}$ from Geneva models (Schaller et al. 1992).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2924_f2.eps} \end{figure}$	Figure 2: The histograms of m_V and B-V for the ELODIE main programme sample stars.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2924_f5.eps} \end{figure}$	Figure 5: The Ca II H line region for the six stars extracted from the co-addition of all spectra available for each star. The 3968.49 Å Ca II H line is indicated by a dotted line. None of the stars exhibits any clear trace of chromospheric emission feature in the line core (see text).
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$\begin{figure} \par\includegraphics[width=14cm,clip]{2924_f6.eps} \end{figure}$	Figure 6: ELODIE radial-velocity measurements in km s $^{\rm -1}$ versus time for all stars but HD 33636 shown in Fig. 7. Each measurement is plotted with an error bar equal to one estimated standard deviation. The orbital solution resulting from the best Keplerian fit, listed in Table 3 and discussed in the text, is superimposed.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{2924_f8.eps} \end{figure}$	Figure 8: $m_{\rm 2} \sin i$ distribution for the 115 planet candidates discovered so far with $m_{\rm 2} \sin i$ < 18 $M_{\rm Jup}$ . The grey square areas point to the contribution of the additional six new candidates presented in this paper.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{2924_f9.eps} \end{figure}$	Figure 9: The location of the 115 planet candidates discovered so far with $m_{\rm 2} \sin i <18~ M_{\rm Jup}$ in the diagram eccentricity versus period. The six new candidates are shown as open triangles.
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