  Solid material in protoplanetary discs will suffer one of two fates after the
epoch of planet formation; either being bound up into planetary bodies, or
remaining in smaller planetesimals to be ground into dust. These end states are
identified through detection of sub-stellar companions by periodic radial
velocity (or transit) variations of the star, and excess emission at mid- and
far-infrared wavelengths, respectively. Since the material that goes into
producing the observable outcomes of planet formation is the same, we might
expect these components to be related both to each other and their host star.
Heretofore, our knowledge of planetary systems around other stars has been
strongly limited by instrumental sensitivity. In this work, we combine
observations at far-infrared wavelengths by IRAS, Spitzer, and Herschel with
limits on planetary companions derived from non-detections in the 16-year
Anglo-Australian Planet Search to clarify the architectures of these
(potential) planetary systems and search for evidence of correlations between
their constituent parts. We find no convincing evidence of such correlations,
possibly owing to the dynamical history of the disk systems, or the greater
distance of the planet-search targets. Our results place robust limits on the
presence of Jupiter analogs which, in concert with the debris disk
observations, provides insights on the small-body dynamics of these nearby
systems.
