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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Gf301_f1.ps} \end{figure}$ Figure 1: Flat, flared and intermediate disk models compared to the observed spectral energy distribution of CFHT-BD-Tau 4. The upper panel has been calculated by using 0.1 astronomical silicate grains, while the lower panel applies 2.0 $\mu$ m olivine and astronomical silicate grains. All model parameters are identical to those in Pascucci et al. (2003), except for the reduced flaring parameter of the intermediate model. The 850 $\mu$ m and 1.3 mm observations are not shown here but fitted well, similarly to Pascucci et al. (2003). The best fit is achieved by the intermediately flaring model in combination with 2 $\mu$ m amorphous olivine grains.
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