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The HD 61005 debris disk ("The Moth") stands out from the growing collectionof spatially resolved circumstellar disks by virtue of its unusual swept-backmorphology, brightness asymmetries, and dust ring offset. Despite severalsuggestions for the physical mechanisms creating these features, no definitiveanswer has been found. In this work, we demonstrate the plausibility of ascenario in which the disk material is shaped dynamically by an eccentric,inclined planet. We present new Keck NIRC2 scattered-light angular differentialimaging of the disk at 1.2-2.3 microns that further constrains its outermorphology (projected separations of 27-135 AU). We also present complementaryGemini Planet Imager 1.6 micron total intensity and polarized light detectionsthat probe down to projected separations less than 10 AU. To test ourplanet-sculpting hypothesis, we employed secular perturbation theory toconstruct parent body and dust distributions that informed scattered-lightmodels. We found that this method produced models with morphological andphotometric features similar to those seen in the data, supporting the premiseof a planet-perturbed disk. Briefly, our results indicate a disk parent bodypopulation with a semimajor axis of 40-52 AU and an interior planet with aneccentricity of at least 0.2. Many permutations of planet mass and semimajoraxis are allowed, ranging from an Earth mass at 35 AU to a Jupiter mass at 5AU.

Bringing "The Moth" to Light: A Planet-Sculpting Scenario for the HD 61005 Debris Disk