All Figures

$\begin{figure} \par\includegraphics[width=6.9cm,clip]{9698fig1.ps}\end{figure}$ Figure 1: Selection of the stable lines from the list provided by Sousa et al. (2007). We present the mean difference between each line abundance and the mean abundance of the respective star as a function of the wavelength. We divided the analysis into three different ranges of effective temperatures. The dashed lines represent the 1.5 sigma threshold. Lines in the shaded area (<4500 Å) were also removed since this region was strongly affected by blending effects, in particular for cooler stars.
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In the text

$\begin{figure} \par\includegraphics[width=6.1cm,clip]{9698fig2.ps}\end{figure}$ Figure 2: In the top panel, we show the distribution of the sample stars in the H-R diagram. The filled circles represent the planet hosts in our sample. We also plot some evolutionary tracks computed with CESAM for a 1.0, 1.1 and 1.2 $M_{\odot }$ . In the bottom panel, we present the metallicity distribution of the sample.
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In the text

$\begin{figure} \par\includegraphics[width=15.8cm,clip]{9698fig3.ps}\end{figure}$ Figure 3: Comparison of our spectroscopic results for the effective temperature with other values found in the literature. We also show the comparison with IRFM using either the Kurucz or Phoenix models.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{9698fig4.ps}\end{figure}$ Figure 4: Comparison of our spectroscopic results for surface gravity with other measurements in the literature.
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In the text

$\begin{figure} \par\includegraphics[width=5.7cm]{9698fig5.ps}\end{figure}$ Figure 5: Comparison of our spectroscopic measurements of [Fe/H] to others found in the literature.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{9698fig6.ps}\end{figure}$ Figure 6: Calibration of the effective temperature as a function of the color index B-V and [Fe/H]. The 3 fitted lines correspond to lines with constant values of [Fe/H] (-0.5, 0.0, 0.5).
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm]{9698fig7.ps}\end{figure}$ Figure 7: Metallicity distribution of jovian planet hosts and neptunian planet hosts within the HARPS GTO ``high precision'' spectroscopic catalogue.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{9698fig8.ps}\end{figure}$ Figure 8: Metallicity distribution for the sample presented in this work (dotted line), for stars hosting neptunian planets (dashed line), and for stars exclusively hosting neptunian planets (full line). The mean metallicity of each distribution is indicated on the plot.
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In the text

$\begin{figure} \par\includegraphics[width=6.1cm,clip]{9698fig2.ps}\end{figure}$	Figure 2: In the top panel, we show the distribution of the sample stars in the H-R diagram. The filled circles represent the planet hosts in our sample. We also plot some evolutionary tracks computed with CESAM for a 1.0, 1.1 and 1.2 $M_{\odot }$ . In the bottom panel, we present the metallicity distribution of the sample.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=15.8cm,clip]{9698fig3.ps}\end{figure}$	Figure 3: Comparison of our spectroscopic results for the effective temperature with other values found in the literature. We also show the comparison with IRFM using either the Kurucz or Phoenix models.
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$\begin{figure} \par\includegraphics[width=15.5cm,clip]{9698fig4.ps}\end{figure}$	Figure 4: Comparison of our spectroscopic results for surface gravity with other measurements in the literature.
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$\begin{figure} \par\includegraphics[width=5.7cm]{9698fig5.ps}\end{figure}$	Figure 5: Comparison of our spectroscopic measurements of [Fe/H] to others found in the literature.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{9698fig6.ps}\end{figure}$	Figure 6: Calibration of the effective temperature as a function of the color index B-V and [Fe/H]. The 3 fitted lines correspond to lines with constant values of [Fe/H] (-0.5, 0.0, 0.5).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.1cm]{9698fig7.ps}\end{figure}$	Figure 7: Metallicity distribution of jovian planet hosts and neptunian planet hosts within the HARPS GTO ``high precision'' spectroscopic catalogue.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{9698fig8.ps}\end{figure}$	Figure 8: Metallicity distribution for the sample presented in this work (dotted line), for stars hosting neptunian planets (dashed line), and for stars exclusively hosting neptunian planets (full line). The mean metallicity of each distribution is indicated on the plot.
Open with DEXTER