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Our analysis of Cassini/VIMS near-infrared spectra of Saturn's Great Storm of2010-2011 reveals a multi-component aerosol composition comprised primarily ofammonia ice, with a significant component of water ice. The most likely thirdcomponent is ammonium hydrosulfide or some weakly absorbing material similar towhat dominates visible clouds outside the storm region. Horizontallyheterogeneous models favor ammonium hydrosulfide as the third component, whilehorizontally uniform models favor the weak absorber. Both models rely on waterice absorption to compensate for residual spectral gradients produced byammonia ice from 3.0 microns to 3.1 microns and need the third component tofill in the sharp ammonia ice absorption peak near 2.96 microns. The bestheterogeneous model has spatial coverage fractions of 55% ammonia ice, 22%water ice, and 23% ammonium hydrosulfide. The best homogeneous model has anoptically thin layer of weakly absorbing particles above an optically thicklayer of water ice particles coated by ammonia ice. This is the firstspectroscopic evidence of water ice in Saturn's atmosphere, found near thelevel of Saturn's visible cloud deck where it could only be delivered bypowerful convection originating from ~200 km deeper in the atmosphere.

Saturn's Great Storm of 2010-2011: Evidence for ammonia and water ices from analysis of VIMS spectra