planetesimals all form as a consequence of agglomeration processes that occur within the protoplanetary disk. Interactions between them during the formation and subsequent evolution leave signs in the disk that can be used to study the current state and past history of a planetary system. Therefore, these faint dusty disks are excellent tools to understand the outer zones of exoplanetary systems including our own.

With sensitive infrared surveys, hundreds of debris disks are known [@matthews14], providing a rich resource to study planetary system evolution and architecture. Although thousands of exoplanets and candidates have been discovered through radial velocity and transit measurements, this breakthrough is currently biased toward the inner zones of systems, not sensitive to planets like Jupiter and Saturn beyond 5 au. Recent improvements in high contrast imaging have enabled us to find planets out at the same stellocentric distance scales as the debris disks. Fomalhaut [@kalas08], HR 8799 [@marois08; @marois10], $\beta$ Pic [@lagrange09], HD 95086 [@rameau13], HD 106906 [@bailey14], and 51 Eri [@machintosh15] are prominent examples of such systems known to host both debris disks and directly imaged planets.

From the observed dust temperatures derived from disk spectral energy distributions (SEDs) of $\sim$200 debris disks, @ballering13 report a 