All Figures

$\begin{figure} { \hbox{ \resizebox{8.7cm}{!}{\includegraphics[angle=90]{4371fg1a... ...}\resizebox{8.7cm}{!}{\includegraphics[angle=90]{4371fg1d.eps}} }}\end{figure}$ Figure 1: Annular averages intensity aperture for the source (solid line) and PSF (dashed line) normalized to the peak value, as a function of radius. The errors drawn are 1 $\sigma$ -errors rms. The reference star for HD 135344 is $\alpha$ Boo, for HD 163296 $\gamma$ Dra, and for CQ Tau, $\beta$ Gem. The plot labeled "2 PSF'' shows two reference stars, $\alpha$ Boo and $\gamma$ Dra, as observed on the March 24, 2000. Although the two reference stars have very different fluxes ( $\gamma$ Dra with 43 Jy and $\alpha$ Boo with 170 Jy, Van Malderen et al. 2004), the two profiles are similar.
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[scale=0.12,angle=90]{4371fg2.eps}} \end{figure}$ Figure 2: Same as Fig. 1, to make a comparison with HD 179218 for which there is no extended emission detected.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4371fg3.eps} \end{figure}$ Figure 3: Annular average intensity aperture normalized to the peak for the observations (full line), model (dashed line), and the PSF associated (dot-dashed line). We have constructed an image with the DD04 model that we have convolved with the PSF of the associated night. The error in the profile comes from the noise rms in the image.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4371fg4.eps} \end{figure}$ Figure 4: Modeled spectrum (dashed line) between 1 and 100 $\mu$ m. For HD 135344 and HD 163296, the ISO spectrum is overplotted by a bold line. For CQ Tau, there are some photometric points from Grady et al. (2005); we have added the one from this study at 20.5 $\mu$ m and IRAS points at 60 and 100 $\mu$ m (filled circles).
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In the text

$\begin{figure} \includegraphics[width=8.2cm,clip]{4371fg5.eps} \end{figure}$ Figure 5: Modelized vertical structure versus the radius. The pressure height scale (H_p/R) is the solid line and the surface height scale (i.e., the height of the disk photosphere above the mid-plane H_s/R) is the dashed line.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4371fg6CMJN.eps} \end{figure}$ Figure 6: HD 163296 extended emission (central point source removed). West is up, north on the left. The pixel size is 0.29 arcsec. The disk has a surface brightness of 0.59 Jy/ $\hbox {$^{\prime \prime }$ }^{2}$ (S/N=27 for $\sigma \sim 0.002$ Jy) for the brightness part in the direction east/west and 0.23 Jy/ $\hbox {$^{\prime \prime }$ }^{2}$ (S/N=11) for the less bright part in the direction north/south. The noise is calculated using a sigma-clipping technique.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4371fg7CMJN.eps} \end{figure}$ Figure 7: CQ Tau extended emission (central point source removed). The same orientation as Fig. 6. The pixel size is 0.29 arcsec. At 0.9 $^{\prime \prime }$ from the center, the surface brightness is 0.94 Jy/ $\hbox {$^{\prime \prime }$ }^{2}$ (S/N=15 for $\sigma \sim 0.004$ Jy). At 2 $^{\prime \prime }$ from the center, the surface brightness is 0.23 Jy/ $\hbox {$^{\prime \prime }$ }^{2}$ (S/N=5).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4371fg8CMJN.eps} \end{figure}$ Figure 8: HD 135344 extended emission (central point source removed). The same orientation as Fig. 6. The pixel size is 0.29 arcsec. At 0.9 $^{\prime \prime }$ from the center, the surface brightness is 0.25 Jy/ $\hbox {$^{\prime \prime }$ }^{2}$ (S/N=15 for $\sigma \sim 0.0015$ Jy).
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[scale=0.12,angle=90]{4371fg2.eps}} \end{figure}$	Figure 2: Same as Fig. 1, to make a comparison with HD 179218 for which there is no extended emission detected.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4371fg3.eps} \end{figure}$	Figure 3: Annular average intensity aperture normalized to the peak for the observations (full line), model (dashed line), and the PSF associated (dot-dashed line). We have constructed an image with the DD04 model that we have convolved with the PSF of the associated night. The error in the profile comes from the noise rms in the image.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4371fg4.eps} \end{figure}$	Figure 4: Modeled spectrum (dashed line) between 1 and 100 $\mu$ m. For HD 135344 and HD 163296, the ISO spectrum is overplotted by a bold line. For CQ Tau, there are some photometric points from Grady et al. (2005); we have added the one from this study at 20.5 $\mu$ m and IRAS points at 60 and 100 $\mu$ m (filled circles).
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$\begin{figure} \includegraphics[width=8.2cm,clip]{4371fg5.eps} \end{figure}$	Figure 5: Modelized vertical structure versus the radius. The pressure height scale (H_p/R) is the solid line and the surface height scale (i.e., the height of the disk photosphere above the mid-plane H_s/R) is the dashed line.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4371fg8CMJN.eps} \end{figure}$	Figure 8: HD 135344 extended emission (central point source removed). The same orientation as Fig. 6. The pixel size is 0.29 arcsec. At 0.9 $^{\prime \prime }$ from the center, the surface brightness is 0.25 Jy/ $\hbox {$^{\prime \prime }$ }^{2}$ (S/N=15 for $\sigma \sim 0.0015$ Jy).
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