All Figures

$\begin{figure} \par\includegraphics[width=17cm,clip]{Gg071_f1.eps} \end{figure}$ Figure 1: Dust flow near a 0.1 ${{M}_{\rm J}}$ planet. Left panel: grey-scale plot of the logarithm of the dust surface density after 400 planetary orbits. Middle panel: logarithm of the dust-to-gas ratio. Right panel: radial cut at $\phi =0$ (opposite to the planet). Solid line: gas surface density, dashed line: dust surface density $\times 100$ . The filled circles indicate the 3:2, the 2:1 and the 3:1 mean motion resonances.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{Gg071_f2.eps} \end{figure}$ Figure 2: Close-up on the gas density near the planet for a high resolution AMR simulation (3 levels of refinement, so a resolution that is 8 times higher than our standard resolution). The arrows indicate the relative velocity of the dust compared to the gas. The typical relative velocity across the shocks is 0.035 $c_{{\rm s}}$ . Note that the color scale is reversed with respect to Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=17.3cm,clip]{Gg071_f3.eps} \end{figure}$ Figure 3: Logarithm of flux densities at 1 mm, normalized by the maximum and convolved with a Gaussian of FWHM 2.5 AU, corresponding to a resolution of 12 mas at 140 pc. Left panel: all particles follow the gas exactly (static dust evolution). Middle panel: particles larger than the critical size decouple from the gas (dynamic dust evolution). Right panel: the corresponding radial flux densities.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{Gg071_f2.eps} \end{figure}$	Figure 2: Close-up on the gas density near the planet for a high resolution AMR simulation (3 levels of refinement, so a resolution that is 8 times higher than our standard resolution). The arrows indicate the relative velocity of the dust compared to the gas. The typical relative velocity across the shocks is 0.035 $c_{{\rm s}}$ . Note that the color scale is reversed with respect to Fig. 1.
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