All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{7646fig1.eps} \end{figure}$ Figure 1: NACO L-band images of HIP 102409 and HIP 107649.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{7646fig2.eps} \end{figure}$ Figure 2: High-pass filtered images of HIP 102409 and HIP 107649.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{7646fig3.eps} \end{figure}$ Figure 3: Difference of HIP 102409 and HIP 107649 with artificial test planets 10 mag fainter than the stars.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{7646fig4.eps} \end{figure}$ Figure 4: Intensity histogram computed from Fig. 3 over a 4 pixel-wide annulus of radius 0.8 $^{\prime \prime }$ containing 804 pixels.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{7646fig5.eps} \end{figure}$ Figure 5: Contrast measured on the high-pass filtered image of HIP 102409 (gray solid line), the PSF-subtracted image of HIP 102409 and HIP 107649 (black solid line) and the 2.8 $^{\prime \prime }$ binary HIP 102141 subtracting the components from each other (black dashed line). At separations larger than 1 $^{\prime \prime }$ to 1.5 $^{\prime \prime }$ , the achievable contrast is limited by sky background rather than stellar residual noise.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{7646fig7.eps} \end{figure}$ Figure 7: NACO L-band images of the 0 $.\!\!^{\prime\prime}$ 65 binary HIP 1910. North is up, East is left.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{7646fig8.eps} \end{figure}$ Figure 8: NACO L-band images of the 0 $.\!\!^{\prime\prime}$ 093 binary GJ 3305. North is up, East is left.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{7646fig9.ps} \end{figure}$ Figure 9: Map of probability that the planet population simulated for a given $\alpha$ and $r_{\rm max}$ value is consistent with the nondetections in our survey.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{7646fig6.ps} \end{figure}$ Figure 6: Discovery space for the observed targets for ages 10 Myr and 30 Myr, except for the older HIP 71395 (500 and 1000 Myr). The shaded area covers the planets that would have been detected by the survey. The field of view in AU is provided as well. The more sensitive lower curve is for the younger age.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{7646fig1.eps} \end{figure}$	Figure 1: NACO L-band images of HIP 102409 and HIP 107649.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{7646fig2.eps} \end{figure}$	Figure 2: High-pass filtered images of HIP 102409 and HIP 107649.
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$\begin{figure} \par\includegraphics[width=5cm,clip]{7646fig3.eps} \end{figure}$	Figure 3: Difference of HIP 102409 and HIP 107649 with artificial test planets 10 mag fainter than the stars.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{7646fig4.eps} \end{figure}$	Figure 4: Intensity histogram computed from Fig. 3 over a 4 pixel-wide annulus of radius 0.8 $^{\prime \prime }$ containing 804 pixels.
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$\begin{figure} \par\includegraphics[width=5cm,clip]{7646fig7.eps} \end{figure}$	Figure 7: NACO L-band images of the 0 $.\!\!^{\prime\prime}$ 65 binary HIP 1910. North is up, East is left.
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$\begin{figure} \par\includegraphics[width=5cm,clip]{7646fig8.eps} \end{figure}$	Figure 8: NACO L-band images of the 0 $.\!\!^{\prime\prime}$ 093 binary GJ 3305. North is up, East is left.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{7646fig9.ps} \end{figure}$	Figure 9: Map of probability that the planet population simulated for a given $\alpha$ and $r_{\rm max}$ value is consistent with the nondetections in our survey.
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$\begin{figure} \par\includegraphics[width=16cm,clip]{7646fig6.ps} \end{figure}$	Figure 6: Discovery space for the observed targets for ages 10 Myr and 30 Myr, except for the older HIP 71395 (500 and 1000 Myr). The shaded area covers the planets that would have been detected by the survey. The field of view in AU is provided as well. The more sensitive lower curve is for the younger age.
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