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We examine the surface brightnesses of Saturn's smaller satellites using aphotometric model that explicitly accounts for their elongated shapes and thusfacilitates comparisons among different moons. Analyses of Cassini imaging datawith this model reveals that the moons Aegaeon, Methone and Pallene are darkerthan one would expect given trends previously observed among the nearbymid-sized satellites. On the other hand, the trojan moons Calypso and Helenehave substantially brighter surfaces than their co-orbital companions Tethysand Dione. These observations are inconsistent with the moons' surfacebrightnesses being entirely controlled by the local flux of E-ring particles,and therefore strongly imply that other phenomena are affecting their surfaceproperties. The darkness of Aegaeon, Methone and Pallene is correlated with thefluxes of high-energy protons, implying that high-energy radiation isresponsible for darkening these small moons. Meanwhile, Prometheus and Pandoraappear to be brightened by their interactions with nearby dusty F ring,implying that enhanced dust fluxes are most likely responsible for Calypso'sand Helene's excess brightness. However, there are no obvious structures in theE ring that would preferentially brighten these two moons, so there must eitherbe something subtle in the E-ring particles' orbital properties that leads toasymmetries in the relevant fluxes, or something happened recently totemporarily increase these moons' brightnesses.

Photometric analyses of Saturn's small moons: Aegaeon, Methone and Pallene are dark; Helene and Calypso are bright