All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{6319fg1.ps} \end{figure}$ Figure 1: Mass ratio vs. semimajor axis of the binary orbit for stars with planets in binary systems. Open circles represent the pairs for which binary orbit is available, open squares the pairs for which only the binary separation is available.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{6319fg2.ps} \end{figure}$ Figure 2: Projected mass vs. orbital period of extrasolar planets. Open circles: single stars; filled circles: binary stars. The size of the symbol is proportional to the critical semimajor axis for dynamical stability (larger symbols refer to the tighter binaries).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{6319fg3a.ps} \includegraphics[width=8cm,clip]{6319fg3b.ps} \end{figure}$ Figure 3: Distribution of the projected mass $m \sin i$ for the planets with period shorter than 40 days and K<15 m/s orbiting single stars (continuous line), planets orbiting binaries with $a_{\rm crit} <75$ AU (dashed line), and planets orbiting binaries with $a_{\rm crit} > 75$ AU (dotted line). Upper panel: histogram; lower panel: cumulative distribution.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6319fg4a.ps} \includegraphics[width=7.8cm,clip]{6319fg4b.ps} \end{figure}$ Figure 4: Distribution of the projected mass $m \sin i$ for the planets with period longer than 40 days orbiting single stars (continous line), planets orbiting binaries with $a_{\rm crit} <75$ AU (dashed line), and planets orbiting binaries with $a_{\rm crit} > 75$ AU (dotted line). Upper panel: histogram; lower panel: cumulative distribution.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6319fg5a.ps} \includegraphics[width=7.8cm,clip]{6319fg5b.ps} \end{figure}$ Figure 5: Distribution of log (period) for the planets orbiting single stars (continous line), planets orbiting binaries with $a_{\rm crit} <75$ AU (dashed line), and planets orbiting binaries with $a_{\rm crit} > 75$ AU (dotted line). Upper panel: histogram; lower panel cumulative distribution.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{6319fg6.ps} \end{figure}$ Figure 6: Eccentricity vs. orbital period for planets in binaries (filled circles) and orbiting single stars (empty circles). Different sizes of filled circles refer to different periastron of the binary orbit (larger sizes: closer orbits).
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{6319fg7a.ps} \includegraphics[width=7.7cm,clip]{6319fg7b.ps} \end{figure}$ Figure 7: Cumulative distribution of the planet eccentricity for the planets with period longer than 40 days orbiting single stars (continous line), planets orbiting binaries with $a_{\rm crit}$ smaller than 75 AU (dashed line), and planets orbiting binaries with $a_{\rm crit}$ larger than 75 AU (dotted line).
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{6319fg8a.ps} \includegraphics[width=7.7cm,clip]{6319fg8b.ps} \end{figure}$ Figure 8: Distribution of the stellar metallicity [Fe/H] for the planets orbiting single stars (continous line), planets orbiting binaries with $a_{\rm crit} <75$ AU (dashed line), and planets orbiting binaries with $a_{\rm crit} > 75$ AU (dotted line). Upper panel: histogram; Lower panel: cumulative distribution.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{6319fg9a.ps} \includegraphics[width=7.7cm,clip]{6319fg9b.ps} \end{figure}$ Figure 9: Distribution of the planet eccentricity for the single planets (continous line), and planets in planetary systems (dotted line). Upper panel: histogram; lower panel: cumulative distribution.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{6319fgA1.ps} \end{figure}$ Figure A.1: Absolute magnitudes and colors for the components of HD 109749 (filled circles). Left panel: M_K vs. V-K; right panel: $M_{\rm J}$ vs. J-K. The 4 Gyr, Z=0.030 isochrone by Girardi et al. (2002) is overplotted.

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{6319fg1.ps} \end{figure}$	Figure 1: Mass ratio vs. semimajor axis of the binary orbit for stars with planets in binary systems. Open circles represent the pairs for which binary orbit is available, open squares the pairs for which only the binary separation is available.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{6319fg2.ps} \end{figure}$	Figure 2: Projected mass vs. orbital period of extrasolar planets. Open circles: single stars; filled circles: binary stars. The size of the symbol is proportional to the critical semimajor axis for dynamical stability (larger symbols refer to the tighter binaries).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{6319fg3a.ps} \includegraphics[width=8cm,clip]{6319fg3b.ps} \end{figure}$	Figure 3: Distribution of the projected mass $m \sin i$ for the planets with period shorter than 40 days and K<15 m/s orbiting single stars (continuous line), planets orbiting binaries with $a_{\rm crit} <75$ AU (dashed line), and planets orbiting binaries with $a_{\rm crit} > 75$ AU (dotted line). Upper panel: histogram; lower panel: cumulative distribution.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6319fg4a.ps} \includegraphics[width=7.8cm,clip]{6319fg4b.ps} \end{figure}$	Figure 4: Distribution of the projected mass $m \sin i$ for the planets with period longer than 40 days orbiting single stars (continous line), planets orbiting binaries with $a_{\rm crit} <75$ AU (dashed line), and planets orbiting binaries with $a_{\rm crit} > 75$ AU (dotted line). Upper panel: histogram; lower panel: cumulative distribution.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6319fg5a.ps} \includegraphics[width=7.8cm,clip]{6319fg5b.ps} \end{figure}$	Figure 5: Distribution of log (period) for the planets orbiting single stars (continous line), planets orbiting binaries with $a_{\rm crit} <75$ AU (dashed line), and planets orbiting binaries with $a_{\rm crit} > 75$ AU (dotted line). Upper panel: histogram; lower panel cumulative distribution.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{6319fg6.ps} \end{figure}$	Figure 6: Eccentricity vs. orbital period for planets in binaries (filled circles) and orbiting single stars (empty circles). Different sizes of filled circles refer to different periastron of the binary orbit (larger sizes: closer orbits).
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{6319fg7a.ps} \includegraphics[width=7.7cm,clip]{6319fg7b.ps} \end{figure}$	Figure 7: Cumulative distribution of the planet eccentricity for the planets with period longer than 40 days orbiting single stars (continous line), planets orbiting binaries with $a_{\rm crit}$ smaller than 75 AU (dashed line), and planets orbiting binaries with $a_{\rm crit}$ larger than 75 AU (dotted line).
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{6319fg8a.ps} \includegraphics[width=7.7cm,clip]{6319fg8b.ps} \end{figure}$	Figure 8: Distribution of the stellar metallicity [Fe/H] for the planets orbiting single stars (continous line), planets orbiting binaries with $a_{\rm crit} <75$ AU (dashed line), and planets orbiting binaries with $a_{\rm crit} > 75$ AU (dotted line). Upper panel: histogram; Lower panel: cumulative distribution.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{6319fg9a.ps} \includegraphics[width=7.7cm,clip]{6319fg9b.ps} \end{figure}$	Figure 9: Distribution of the planet eccentricity for the single planets (continous line), and planets in planetary systems (dotted line). Upper panel: histogram; lower panel: cumulative distribution.
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