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Protoplanetary disks are a byproduct of the star formation process. In thedense mid-plane of these disks, planetesimals and planets are expected to form.The first step in planet formation is the growth of dust particles fromsubmicrometer-sized grains to macroscopic mm-sized aggregates. The grain growthis accompanied by radial drift and vertical segregation of the particles withinthe disk. To understand this essential evolutionary step, spatially resolvedmulti-wavelength observations as well as photometric data are necessary whichreflect the properties of both disk and dust. We present the first spatiallyresolved image obtained with NACO at the VLT in the L$_\text{p}$ band of thenear edge-on protoplanetary disk FS Tau B. Based on this new image, apreviously published Hubble image in H band and the spectral energydistribution from optical to millimeter wavelengths, we derive constraints onthe spatial dust distribution and the progress of grain growth. For thispurpose we perform a disk modeling using the radiative transfer code MC3D.Radial drift and vertical sedimentation of the dust are not considered. We finda best-fit model which features a disk extending from $2\,\text{AU}$ to severalhundreds AU with a moderately decreasing surface density and$M_\text{disk}=2.8\,\times\,10^{-2}\,\text{M}_\odot$. The inclination amountsto $i=80^\circ$. Our findings indicate that substantial dust grain growth hastaken place and that grains of a size equal to or larger than $1\,\text{mm}$are present in the disk. In conclusion, the parameters describing the verticaldensity distribution are better constrained than those describing the radialdisk structure.

The circumstellar disk of FS Tau B - A self-consistent model based on observations in the mid-infrared with NACO -