  Compact systems of multiple close-in super-Earths/sub-Neptunes ("compact
multis") are a ubiquitous outcome of planet formation. It was recently
discovered that the outer edges of compact multis are located at smaller
orbital periods than expected from geometric and detection biases alone,
suggesting some truncation or transition in the outer architectures. Here we
test whether this "edge-of-the-multis" might be explained in any part by
distant giant planets in the outer regions ($\gtrsim 1$ AU) of the systems. We
investigate the dynamical stability of observed compact multis in the presence
of hypothetical giant ($\gtrsim 0.5 \ M_{\mathrm{Jup}}$) perturbing planets. We
identify what parameters would be required for hypothetical perturbing planets
if they were responsible for dynamically sculpting the outer edges of compact
multis. "Edge-sculpting" perturbers are generally in the range $P\sim100-500$
days for the average compact multi, with most between $P\sim200-300$ days.
Given the relatively close separation, we explore the detectability of the
hypothetical edge-sculpting perturbing planets, finding that they would be
readily detectable in transit and radial velocity data. We compare to
observational constraints and find it unlikely that dynamical sculpting from
distant giant planets contributes significantly to the edge-of-the-multis.
However, this conclusion could be strengthened in future work by a more
thorough analysis of the detection yields of the perturbing planets.
