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The 27 satellites of Uranus are enigmatic, with dark surfaces coated bymaterial that could be rich in organics. Voyager 2 imaged the southernhemispheres of Uranus' five largest 'classical' moons Miranda, Ariel, Umbriel,Titania, and Oberon, as well as the largest ring moon Puck, but their northernhemispheres were largely unobservable at the time of the flyby and were notimaged. Additionally, no spatially resolved datasets exist for the other 21known moons, and their surface properties are essentially unknown. BecauseVoyager 2 was not equipped with a near-infrared mapping spectrometer, ourknowledge of the Uranian moons' surface compositions, and the processes thatmodify them, is limited to disk-integrated datasets collected by ground- andspace-based telescopes. Nevertheless, images collected by the Imaging ScienceSystem on Voyager 2 and reflectance spectra collected by telescope facilitiesindicate that the five classical moons are candidate ocean worlds that mightcurrently have, or had, liquid subsurface layers beneath their icy surfaces. Todetermine whether these moons are ocean worlds, and investigate Uranus' ringmoons and irregular satellites, close-up observations and measurements made byinstruments onboard a Uranus orbiter are needed.

The science case for spacecraft exploration of the Uranian satellites: Candidate ocean worlds in an ice giant system