Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{0469f1.eps}\end{figure}$ Figure 1: Comparison of the $T_{{\rm eff}}$ values derived in this work with the ones obtained by other authors for the same stars. The solid line represents a 1:1 relation. See text for more details.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0469f2.eps}\end{figure}$ Figure 2: Comparison of the spectroscopic $\log{g}$ values derived in this work with the ones obtained by other authors for the same stars. The solid line represents a 1:1 relation. See text for more details.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0469f3.eps}\end{figure}$ Figure 3: Comparison of the spectroscopic and parallax based surface gravities of our program stars. Filled symbols represent planet-host stars, while open symbols denote stars from our comparison sample. The error bars represent typical relative errors in both axis. The solid line represents a 1:1 relation.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0469f4.eps}\end{figure}$ Figure 4: Comparison of the [Fe/H] values derived in this work with the ones obtained by other authors for the same stars. The solid line represents a 1:1 relation. See text for more details.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0469f5.eps}\end{figure}$ Figure 5: Metallicity as a function of the effective temperature for planet hosts (filled dots) and comparison sample stars (open circles). The dotted line represents the approximate lower limit in B-V of the CORALIE planet search sample (Udry et al. 2000), as based on Eq. (A.1) (for B-V= constant = 0.5).
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{0469f6.eps}\end{figure}$ Figure 6: Upper panels: [Fe/H] distributions for planet host stars (hashed histogram) and for our volume-limited comparison sample of stars (open bars). The average difference between the [Fe/H] of the two samples is of $\sim$ 0.25 dex. A Kolgomorov-Smirnov test shows that the probability that the two samples are part of the same population is of the order of 10^-9. See text for more details. Lower panel, left: [Fe/H] distributions for planet host stars (hashed histogram) included in the CORALIE planet-search sample, when compared with the same distribution for all the 875 stars in the whole CORALIE program for which we have at least 5 radial-velocity measurements (solid-line open histogram). Lower panel, right: percentage of planet hosts found amid the stars in the CORALIE sample as a function of stellar metallicity.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{0469f7.eps}\end{figure}$ Figure 7: Percentage of planet hosts for the plot in Fig. 6 (lower-right panel, hashed histogram) as a function of the mass fraction of heavy elements (an increasing function of [Fe/H]). Error bars are approximate values based on Gaussian statistics. The plot suggests that the percentage is relatively constant for Z < 0.02 (solar), increasing then linearly for higher Z values, with an increase of 16% for each $\Delta Z=$ 0.01.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{0469fa1.eps}\end{figure}$ Figure A.1: Calibration of the $T_{{\rm eff}}$ as a function of B-V and [Fe/H]. The 5 "fitted'' lines represent lines of constant [Fe/H] (in steps of 0.3 dex).

In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{0469fa2.eps}\end{figure}$ Figure A.2: Comparison between the effective temperatures derived from our calibration and the one of Alonso et al. (1996). The dotted line represents a 1:1 relation while the solid line is a linear fit to the points.

In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{0469f1.eps}\end{figure}$	Figure 1: Comparison of the $T_{{\rm eff}}$ values derived in this work with the ones obtained by other authors for the same stars. The solid line represents a 1:1 relation. See text for more details.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{0469f2.eps}\end{figure}$	Figure 2: Comparison of the spectroscopic $\log{g}$ values derived in this work with the ones obtained by other authors for the same stars. The solid line represents a 1:1 relation. See text for more details.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0469f3.eps}\end{figure}$	Figure 3: Comparison of the spectroscopic and parallax based surface gravities of our program stars. Filled symbols represent planet-host stars, while open symbols denote stars from our comparison sample. The error bars represent typical relative errors in both axis. The solid line represents a 1:1 relation.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0469f4.eps}\end{figure}$	Figure 4: Comparison of the [Fe/H] values derived in this work with the ones obtained by other authors for the same stars. The solid line represents a 1:1 relation. See text for more details.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0469f5.eps}\end{figure}$	Figure 5: Metallicity as a function of the effective temperature for planet hosts (filled dots) and comparison sample stars (open circles). The dotted line represents the approximate lower limit in B-V of the CORALIE planet search sample (Udry et al. 2000), as based on Eq. (A.1) (for B-V= constant = 0.5).
Open with DEXTER