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Although the architectures of compact multiple-planet systems arewell-characterized, there has been little examination of their "outer edges",or the locations of their outermost planets. Here we present evidence that theobserved high-multiplicity Kepler systems truncate at smaller orbital periodsthan can be explained by geometric and detection biases alone. To show this, weconsidered the existence of hypothetical planets orbiting beyond the observedtransiting planets with properties dictated by the "peas-in-a-pod" patterns ofintra-system radius and period ratio uniformity. We evaluated the detectabilityof these hypothetical planets using (1) a novel approach for estimating themutual inclination dispersion of multi-transiting systems based on transitchord length ratios and (2) a model of transit probability and detectionefficiency that accounts for the impacts of planet multiplicity oncompleteness. Under the assumption that the "peas-in-a-pod" patterns continueto larger orbital separations than observed, we find that $\gtrsim35\%$ ofKepler compact multis should possess additional detected planets beyond theknown planets, constituting a $\sim7\sigma$ discrepancy with the lack of suchdetections. These results indicate that the outer ($\sim100-300$ days) regionsof compact multis experience a truncation (i.e. an "edge-of-the-multis") or asignificant breakdown of the "peas-in-a-pod" patterns, in the form ofsystematically smaller radii or larger period ratios. We outline futureobservations that can distinguish these possibilities, and we discussimplications for planet formation theories.

Edge-of-the-Multis: Evidence for a Transition in the Outer Architectures of Compact Multi-Planet Systems