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W. M. Grundy, M. W. Buie, J. R. Spencer, J. A. Stansberry (Lowell Obs.), B. Schmitt (CNRS/LGGE), C. Dalla Piazza (Lycoming Col.), B. N. Hilbert (Boston Univ.)
We have obtained spectra of a large sample of outer solar system objects using the OSIRIS spectrometer, covering the wavelength range from 1.2 to 2.3~\mum. Our spectra of many of the solid objects exhibit near-IR absorptions bands characteristic of low-temperature, crystalline water ice. These objects include satellites of Jupiter, Saturn, and Uranus, as well as the rings of Saturn. We make use of new H2O ice optical constants [Grundy and Schmitt 1998 {\it J.\ Geophs.\ Res.} in press.] to analyze our spectra to determine the physical state and temperature of H2O ice at the surfaces of these objects.
We will present the technique we have developed for determining temperatures of ice-rich surfaces from near-IR spectra, and will discuss limitations of this technique which result from effects such as multiple scattering, radiation damage, and the presence of hydrated impurities. Under some circumstances, these effects can result in errors in the derived temperature.
We will also discuss the application of our technique to remote sensing of temperature changes, which are less vulnerable to errors resulting from the effects listed above.
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