All Figures

$\begin{figure} \par\psfrag{Angle}[c][c]{Position angle ($^\circ$ )} \psfrag{Int... ...Normalized intensity} \includegraphics[width=8.8cm]{7137fig1.eps} \end{figure}$ Figure 1: Azimuthal brightness profiles of the best model without stratification (solid line) superimposed to observed profiles (triangles). The model parameters are p = -5.5 and $a_\textrm{max} = 100~\mu$ m. The position angle $0^\circ$ corresponds to the disk semi-minor axis, on the front face of the ring.
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In the text

$\begin{figure} \par\psfrag{proba}[c][c]{Probability} \psfrag{p}[c][c]{$p$ } \p... ...c][c]{$a_{\rm max}$ } \includegraphics[width=8.8cm]{7137fig2.eps} \end{figure}$ Figure 2: Bayesian probability distribution in the non-stratified case for grain size distribution slope ( left) and maximum grain size ( right).
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In the text

$\begin{figure} \par\includegraphics[angle=190,width=4.5cm,clip]{7137fig3.eps} %\end{figure}$ Figure 3: Synthetic image of the GG Tau ring in the I band with only vertical stratification. The color map is in logarithmic scale and is inverted with bright regions in dark. The image size is 3.7 arcsec.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{7137fig4.eps} \end{figure}$ Figure 4: Sketch of the vertical and radial stratification proposed to account for the scattered light images of GG Tau.
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In the text

$\begin{figure} \par\psfrag{Angle}[c][c]{Position angle ($^\circ$ )} \psfrag{Int... ...Normalized intensity} \includegraphics[width=8.8cm]{7137fig5.eps} \end{figure}$ Figure 5: Azimuthal brightness profiles of the best model with stratification (solid line) superimposed to observed profiles (triangles). The model parameters are $\xi = 0.15$ and $a_\textrm{max} = 60~\mu$ m.
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In the text

$\begin{figure} \par\psfrag{proba}[c][c]{Probability} \psfrag{strat}[c][c]{Strat... ...c][c]{$a_{\rm max}$ } \includegraphics[width=8.8cm]{7137fig6.eps} \end{figure}$ Figure 6: Bayesian probability distribution in the stratified case.
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In the text

$\begin{figure} \psfrag{pola}[c][c]{Linear polarisation level} \psfrag{angle}[c... ...on angle ($^\circ$ )} \includegraphics[width=8.8cm]{7137fig7.eps} \end{figure}$ Figure 7: Observed (from Silber et al. 2000) and synthetic polarisation at 1 $\mu$ m as a function of the azimuthal angle. Polarisation maps have been binned by a factor 4, resulting in a pixel size of 0.172 $^{\prime \prime }$ and then divided in 20 $^\circ$ sectors where the polarisation is measured, for each sector, in the pixel of maximum brightness. Black circles represent the polarisation extracted from observations. The solid red line corresponds to the best model with stratification and a slope p=-3.5 and the dashed blue line to the model without stratification and a slope p=-5.5. The position angle $0^\circ$ is defined as in the previous figures and corresponds to the disk semi-minor axis, on the front side of the disk.
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In the text

$\begin{figure} \resizebox{8.8cm}{!}{ \includegraphics{7137fig8.eps} } \end{figure}$ Figure 8: Density contours for dust ( left) and gas ( right) at the end of the SPH simulations of the circumbinary disk for runs including 10, 5 and 1 $\mu$ m grains from top to bottom.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{7137fig9.eps} \end{figure}$ Figure 9: Fits for the 5 $\mu$ m dust particles in the circumbinary disk. a) Scaleheight. b) Surface density. In both cases, the dotted line corresponds to the vertical fit only and the solid line to the subsequent radial fit. c) SPH density after smoothing on a regular grid. d) Vertical fit of the density. e) Complete fit of the density in both vertical and radial directions.
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In the text

$\begin{figure} \par\includegraphics[width=4.4cm,clip]{7137fig10.eps}\includegraphics[width=4.4cm,clip]{7137fig11.eps} \end{figure}$ Figure 10: Scaleheight ( left) and surface density ( right) for the small grains (1 to 10 $\mu$ m) in the circumbinary disk.
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In the text

$\begin{figure} \par\psfrag{intensite normalisee}[c][c]{Normalized intensity} \p... ...e L'}[c][c]{L' band} \includegraphics[width=8.8cm]{7137fig12.eps} \end{figure}$ Figure 11: Azimuthal brightness profiles of the circumbinary disk with (solid line) and without (dashed line) stratification superimposed to GG Tau's observed profiles (triangles).
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In the text

$\begin{figure} \par\psfrag{Angle}[c][c]{Position angle ($^\circ$ )} \psfrag{Int... ...Normalized intensity} \includegraphics[width=8.8cm]{7137fig1.eps} \end{figure}$	Figure 1: Azimuthal brightness profiles of the best model without stratification (solid line) superimposed to observed profiles (triangles). The model parameters are p = -5.5 and $a_\textrm{max} = 100~\mu$ m. The position angle $0^\circ$ corresponds to the disk semi-minor axis, on the front face of the ring.
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$\begin{figure} \par\psfrag{proba}[c][c]{Probability} \psfrag{p}[c][c]{$p$ } \p... ...c][c]{$a_{\rm max}$ } \includegraphics[width=8.8cm]{7137fig2.eps} \end{figure}$	Figure 2: Bayesian probability distribution in the non-stratified case for grain size distribution slope ( left) and maximum grain size ( right).
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$\begin{figure} \par\includegraphics[angle=190,width=4.5cm,clip]{7137fig3.eps} %\end{figure}$	Figure 3: Synthetic image of the GG Tau ring in the I band with only vertical stratification. The color map is in logarithmic scale and is inverted with bright regions in dark. The image size is 3.7 arcsec.
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{7137fig4.eps} \end{figure}$	Figure 4: Sketch of the vertical and radial stratification proposed to account for the scattered light images of GG Tau.
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$\begin{figure} \par\psfrag{Angle}[c][c]{Position angle ($^\circ$ )} \psfrag{Int... ...Normalized intensity} \includegraphics[width=8.8cm]{7137fig5.eps} \end{figure}$	Figure 5: Azimuthal brightness profiles of the best model with stratification (solid line) superimposed to observed profiles (triangles). The model parameters are $\xi = 0.15$ and $a_\textrm{max} = 60~\mu$ m.
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$\begin{figure} \par\psfrag{proba}[c][c]{Probability} \psfrag{strat}[c][c]{Strat... ...c][c]{$a_{\rm max}$ } \includegraphics[width=8.8cm]{7137fig6.eps} \end{figure}$	Figure 6: Bayesian probability distribution in the stratified case.
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$\begin{figure} \resizebox{8.8cm}{!}{ \includegraphics{7137fig8.eps} } \end{figure}$	Figure 8: Density contours for dust ( left) and gas ( right) at the end of the SPH simulations of the circumbinary disk for runs including 10, 5 and 1 $\mu$ m grains from top to bottom.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{7137fig9.eps} \end{figure}$	Figure 9: Fits for the 5 $\mu$ m dust particles in the circumbinary disk. a) Scaleheight. b) Surface density. In both cases, the dotted line corresponds to the vertical fit only and the solid line to the subsequent radial fit. c) SPH density after smoothing on a regular grid. d) Vertical fit of the density. e) Complete fit of the density in both vertical and radial directions.
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$\begin{figure} \par\includegraphics[width=4.4cm,clip]{7137fig10.eps}\includegraphics[width=4.4cm,clip]{7137fig11.eps} \end{figure}$	Figure 10: Scaleheight ( left) and surface density ( right) for the small grains (1 to 10 $\mu$ m) in the circumbinary disk.
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$\begin{figure} \par\psfrag{intensite normalisee}[c][c]{Normalized intensity} \p... ...e L'}[c][c]{L' band} \includegraphics[width=8.8cm]{7137fig12.eps} \end{figure}$	Figure 11: Azimuthal brightness profiles of the circumbinary disk with (solid line) and without (dashed line) stratification superimposed to GG Tau's observed profiles (triangles).
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