Spectroscopic Search for Water Ice on Jovian Trojan Asteroids

Details Spectroscopic Search for Water Ice on Jovian Trojan Asteroids Spectroscopic Search for Water Ice on Jovian Trojan Asteroids

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.5003y&link_type=abstract

American Astronomical Society, DPS meeting #38, #50.03; Bulletin of the American Astronomical Society, Vol. 38, p.577

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Scientific paper

We are conducting a systematic study of the Jovian Trojans using the Subaru 8-m, UKIRT 4-m and IRTF 3-m telescopes atop Mauna Kea, Hawaii. Theoretical models show that the Jovian Trojans formed beyond the snow-line and they may contain considerable amounts of water ice. We seek spectroscopic evidence for this pristine ice.
Object (4709) Ennomos has a geometric albedo of 0.13+/-0.02, which is significantly above the mean Trojan albedo of 0.041+/- 0.002 (Fernandez et al., 2003). An intriguing possibility is that the albedo of Ennomos is high because a recent impact has coated part of the surface with freshly excavated ice. We obtained near-IR (0.8-2.5 micron) spectra of (4709) Ennomos in search of the 1.5 and 2.0
micron bands of water ice. Four other Trojans, (911) Agamemnon, (617) Patroclus, (1143) Odysseus and (2797) Teucer, were also observed. These objects have been reported to show possible weak absorptions at 1.7 and 2.3 micron respectively (Emery and Brown, 2003). All five targets appear spectrally featureless, even in our
highest signal-to-noise ratio data. We present the data and a simple model consisting of mixtures of water ice and a spectrally featureless material, to quantify the limits to surface ice.

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