Since Saturn orbit insertion on July 1, 2004, Cassini's Visual and Infrared Mapping Spectrometer (VIMS) has been observing the planet, its rings, Titan and several icy satellites, obtaining both images and spectra in the 1-5 micron region. I will review some of the highlights of these observations, concentrating on Saturn and its spectacular ring system. VIMS spectra reveal the ring particles to be covered by almost pure water frost, with typical grain sizes of 10-100 microns. An as-yet unidentified contaminant which gives the rings their reddish visible color --- possibly complex organic molecules known as tholins --- seems to be located within the ice grains themselves. In 2005 we observed four occultations by Saturn's rings of the long-period variable star, o Ceti (Mira). Large, systematic variations in the transmission of the A ring with longitude seen in these data are consistent with both the well-known azimuthal asymmetry in reflected light, as well as asymmetries seen in radar images of the rings obtained at Arecibo. The most probable cause of all these phenomena is a pattern of unresolved `self-gravity wakes' in the A ring. A simple model of the wakes permits us to make a new estimate of the vertical thickness of the rings of about 5m, a result which is consistent with --- but significantly less than --- previous experimental determinations. The VIMS occultations have also provided new data on the enigmatic, multi-stranded F ring; on several tenuous ringlets which inhabit the Encke Gap and Cassini Division; and on the many density waves driven in the rings by external satellites. Most exciting, but as yet imperfectly understood, is a systematic enhancement in the statistical noise present in some ring regions which we attribute to the intrinsic `graininess' of the rings at 10-100 meters.