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Resolved debris disk features (e.g., warps, offsets, edges and gaps,azimuthal asymmetries, radially thickened rings, scale heights) containvaluable information about the underlying planetary systems, such as theposited planet's mass, semi-major axis, and other orbital parameters. Mostexisting models assume a single planet is sculpting the disk feature, butrecent observations of mature planetary systems (e.g., by radial velocitysurveys or \textit{Kepler}) have revealed that many planets reside inmulti-planet systems. Here we investigate if/how planet properties inferredfrom single-planet models are compromised when multiple planets reside in thesystem. For each disk feature, we build a two-planet model that includes aplanet b with fixed parameters and a planet c with a full range of possibleparameters. We investigate these two-planet systems and summarize theconfigurations for which assuming a single planet (i.e., planet b) leads tosignificantly flawed inferences of that planet's properties. We find thatalthough disk features are usually primarily dominated by a single planet, whenusing single-planet models we are at risk of misinterpreting planet propertiesby orders of magnitude in extreme cases. Specifically, we are at high risk ofmisinterpreting planet properties from disk warps; at moderate risk from diskedges and gaps, radially thickened rings, and scale height features; and at lowrisk from host star-disk center offsets and azimuthal asymmetries. We summarizesituations where we can infer the need to use a multi-planet model instead of asingle-planet one from disk morphology dissimilarities.

Debris Disks in Multi-Planet Systems: Are Our Inferences Compromised by Unseen Planets?