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The recent progress in instrumentation and telescope development has broughtus different ways to observe protoplanetary disks, including interferometers,space missions, adaptive optics, polarimetry, and time- and spectrally-resolveddata. While the new facilities have changed the way we can tackle the existingopen problems in disk structure and evolution, there is a substantial lack ofinterconnection between different observing techniques and their usercommunities. Here, we explore the complementarity of some of thestate-of-the-art observing techniques, and how they can be brought together ina collective effort to understand how disks evolve and disperse at the time ofplanet formation.  This paper was born at the "Protoplanetary Discussions" meeting in Edinburgh,2016. Its goal is to clarify where multi-wavelength observations of disksconverge in unveiling disk structure and evolution, and where they diverge andchallenge our current understanding. We discuss caveats that should beconsidered when linking results from different observations, or when drawingconclusions based on limited datasets (in terms of wavelength or sample). Wefocus on disk properties that are currently being revolutionized bymulti-wavelength observations. Specifically: the inner disk radius, holes andgaps and their link to large-scale disk structures, the disk mass, and theaccretion rate. We discuss how the links between them, as well as the apparentcontradictions, can help us to disentangle the disk physics and to learn aboutdisk evolution.

A "Rosetta Stone" for protoplanetary disks: The synergy of multi-wavelength observations