Abstract
We review relatively recent spectroscopic remote sensing observations, from Earth‐based telescopes, that have been used to identify condensed volatile ices on the surfaces of satellites in the Jovian, Saturnian, and Uranian systems, Neptune’s moon Triton, Pluto, and Pluto’s satellite Charon. Water ice appears ubiquitous on the surfaces of the larger satellites in the Jovian, Saturnian, and Uranian systems and on Charon. More volatile species of ices appear to dominate the surfaces of Triton (N2, CO, CH4, and CO2) and Pluto (N2, CO, and CH4).
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