Near Infreared Spectroscopy of Kuiper Belt Objects: More than Just Water Ice

Astronomy and Astrophysics – Astronomy

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Remote sensing via near-infrared (NIR) spectroscopy is the only method available to examine the surface composition of Kuiper Belt Objects (KBOs). Crystalline water ice, which requires T > 100 K for formation, has been observed on several KBOs including Charon. In addition to water ice, ammonia hydrates have also been seen on Charon (Cook et al., 2007) and possibly Quaoar (Jewitt & Luu, 2004). Both ices have relatively short lifetimes (< 30 Myr, Cook et al., 2007) when exposed on the surface and require a renewal mechanism such as cryovolcanism (Cook et al., 2007). We will discuss NIR spectra of Quaoar and Orcus obtained from the Subaru, VLT and Gemini North archives. Besides crystalline water ice, the spectrum of Quaoar clearly shows evidence for ammonia hydrate at 2.21 μm. Data obtained over several nights suggest that this feature shifts in wavelength, as seen on Charon (Cook et al., 2007). We also see two unidentified features in the spectrum of Quaoar at 1.33 and 1.80 μm, which we tentatively identify as hydrated materials such as phyllosilicates or salts. The spectrum of Orcus, which has crystalline water ice (de Bergh et al., 2005), we find also shows evidence, though less certain, for a feature around 2.23 μm, which may be due to a mixture of pure ammonia ice and ammonia hydrate. This feature may be correlated with Orcus's rotation, further suggesting a patchy surface. Quaoar and Orcus are similar in radius, presumably mass, and spectral characteristics to Charon. Comparative studies of these three objects may tell us more about KBOs than studying them individually.

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