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The solar system's Zodiacal Cloud is visible to the unaided eye, yet theorigin of its constituent dust particles is not well understood, with a widerange of proposed divisions between sources in the asteroid belt and JupiterFamily comets. The amount of dust contributed by Oort Cloud comets isuncertain. Knowledge of the Zodiacal Cloud's structure and origins would helpwith NASA's aim of characterizing potentially Earth-like planets around nearbystars, since the exo-Earths must be studied against the light scattered fromextrasolar analogs of our cloud. As the only example where the parent bodiescan be tracked, our own cloud is critical for learning how planetary systemarchitecture governs the interplanetary dust's distribution. Our cloud has beenrelatively little-studied in the near-ultraviolet, a wavelength range that isimportant for identifying potentially-habitable planets since it contains thebroad Hartley absorption band of ozone. We show through radiative transfermodeling that our cloud's shape and size at near-UV wavelengths can be measuredfrom Earth orbit by mapping the zodiacal light's flux and linear polarizationacross the sky. We quantify how well the cloud's geometric and opticalproperties can be retrieved from a set of simulated disk observations, using aMarkov chain Monte Carlo analysis. The results demonstrate that observationswith sufficient precision, covering a set of fields distributed along theecliptic and up to the poles, can be used to determine the division betweenasteroidal, Jupiter Family, and Oort Cloud dust components, primarily via theirdiffering orbital inclination distributions. We find that the observations mustbe repeated over a time span of several months in order to disentangle thezodiacal light from the Galactic background using the Milky Way's rotationacross the sky.

Determining the Shape, Size, and Sources of the Zodiacal Dust Cloud using Polarized Ultraviolet Scattered Sunlight