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Grain growth in protoplanetary disks is the first step towards the formationof the rocky cores of planets. Models predict that grains grow, migrate, andfragment in the disk and predict varying dust properties as a function ofradius, age, and physical properties. High-angular resolution observations atmore than one (sub-)mm wavelength are the essential tool for constraining graingrowth and migration on the disk midplane. We developed a procedure to analyzeself-consistently multi wavelength (sub-)mm continuum interferometricobservations of protoplanetary disks to constrain the radial distribution ofdust properties. We apply this technique to existing multi frequency continuummm observations of the disk around CQ Tau, a A8 pre-main sequence star with awell-studied disk. We demonstrate that our models can be used to simultaneouslyconstrain the disk and dust structure. In CQ Tau, the best-fitting model has aradial dependence of the maximum grain size, which decreases from a few cm inthe inner disk (<40 AU) to a few mm at 80 AU. Nevertheless, the currentlyavailable dataset does not allow us to exclude the possibility of a uniformgrain size distribution at a 3sigma level.

Constraints on the radial distribution of the dust properties in the CQ Tau protoplanetary disk