All Figures

$\begin{figure} \par\includegraphics[width=5.85cm,clip]{4534f1a.eps}\hspace*{4mm}... ...c.eps}\hspace*{4mm} \includegraphics[width=5.85cm,clip]{4534f1d.eps}\end{figure}$ Figure 1: Abundance ratios [X/H] plotted vs. the elemental condensation temperatures $T_{\rm C}$ for the planet host HD 20367 and HD 39091 ( left panels), and for the comparison sample stars HD 23484 and HD 69830 ( right panels). The solid lines represent the linear least-squares fits to the data. The slopes values and the typical error bars associated with the [X/H] ratios are indicated at the bottom and the top of each plot, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4534f2.eps}\end{figure}$ Figure 2: Slopes derived from [X/H] vs. $T_{\rm C}$ for all the planet host ( filled symbols) and comparison sample ( open symbols) stars. The solid lines represent the average slope of the two samples, and the average slope $\pm$ one standard deviation. The dotted and dashed lines indicate the average slope of stars with and without planets, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4534f3.eps}\end{figure}$ Figure 3: [X/H] vs. $T_{\rm C}$ slopes plotted vs. [Fe/H] for all the planet host ( filled symbols) and comparison sample ( open symbols) stars. The solid lines represent the linear least-squares fit $\pm$ 2 $\sigma$ for all the targets, while the dotted and dashed lines indicate the linear least-squares fits $\pm$ 2 $\sigma$ for stars with and without planets, respectively. The slopes of each linear fit are shown at the bottom.
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In the text

$\begin{figure} \par\includegraphics[width=5.85cm,clip]{4534f4a.eps}\hspace*{4mm} \includegraphics[width=5.85cm,clip]{4534f4b.eps}\end{figure}$ Figure 4: Abundance ratios [X/H] plotted vs. the elemental condensation temperatures $T_{\rm C}$ for the planet host stars HD 169830 and HD 114783, having $T_{\rm C}$ slopes more than 2 $\sigma$ below the $T_{\rm C}$ slopes vs. [Fe/H] fit. The solid lines represent the linear least-squares fits to the data. The slopes values and the typical error bars associated with the [X/H] ratios are indicated at the bottom and the top of each plot, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=5.85cm,clip]{4534f5a.eps}\hspace*{4mm} \includegraphics[width=5.85cm,clip]{4534f5b.eps}\end{figure}$ Figure 5: [X/H] vs. $T_{\rm C}$ slopes plotted vs. $T_{\rm eff}$ for all the planet host ( filled symbols) and comparison sample ( open symbols) stars.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4534f6.eps}\end{figure}$ Figure 6: [X/H] vs. $T_{\rm C}$ slopes plotted vs. the planetary mass in $M_{\rm J}$ units ( left panel) and the planetary period in days ( right panel) for all the planets: b components ( filled symbols) and c, d, ... components of planetary systems ( open symbols). The lower panels show the standarddeviations per bin corresponding to the above representations.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4534f7.eps}\end{figure}$ Figure 7: [X/H] vs. $T_{\rm C}$ slopes plotted vs. the orbital semi-major axis in AU ( left panel) and the orbital eccentricity ( right panel) for all the planets: b components ( filled symbols) and c, d, ... components of planetary systems ( open symbols). The lower panels show the standard deviations per bin corresponding to the above representations.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4534f2.eps}\end{figure}$	Figure 2: Slopes derived from [X/H] vs. $T_{\rm C}$ for all the planet host ( filled symbols) and comparison sample ( open symbols) stars. The solid lines represent the average slope of the two samples, and the average slope $\pm$ one standard deviation. The dotted and dashed lines indicate the average slope of stars with and without planets, respectively.
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$\begin{figure} \par\includegraphics[width=5.85cm,clip]{4534f5a.eps}\hspace*{4mm} \includegraphics[width=5.85cm,clip]{4534f5b.eps}\end{figure}$	Figure 5: [X/H] vs. $T_{\rm C}$ slopes plotted vs. $T_{\rm eff}$ for all the planet host ( filled symbols) and comparison sample ( open symbols) stars.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4534f6.eps}\end{figure}$	Figure 6: [X/H] vs. $T_{\rm C}$ slopes plotted vs. the planetary mass in $M_{\rm J}$ units ( left panel) and the planetary period in days ( right panel) for all the planets: b components ( filled symbols) and c, d, ... components of planetary systems ( open symbols). The lower panels show the standarddeviations per bin corresponding to the above representations.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4534f7.eps}\end{figure}$	Figure 7: [X/H] vs. $T_{\rm C}$ slopes plotted vs. the orbital semi-major axis in AU ( left panel) and the orbital eccentricity ( right panel) for all the planets: b components ( filled symbols) and c, d, ... components of planetary systems ( open symbols). The lower panels show the standard deviations per bin corresponding to the above representations.
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