Abstract
In this lecture, I will review the properties of protoplanetary disks as derived from high angular resolution observations. I discuss how the combination of several different high angular resolution techniques allow us to probe different regions of the disk and to derive the properties of the dust when combined with sophisticated disk models. The picture that emerges is that the dust in circumstellar disks surrounding pre-main sequence stars is in many cases significantly evolved compared to the dust in molecular clouds and the interstellar medium. It is, however, still difficult to derive a consistent picture and timeline for dust evolution in disks, as the observations are still limited to small samples of objects.
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