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Spectroscopic Search for Water Ice on Jovian Trojan Asteroids
The Jovian Trojans likely formed beyond the snow line and so may containconsiderable amounts of water ice. We seek near-infrared spectroscopicevidence for the 1.5 and 2.0 ?m water ice bands in the Trojans. Oursample is focused on objects identified in previous measurements asbeing of special interest. The unusual Trojan (4709) Ennomos has ageometric albedo significantly above the mean Trojan albedo, perhapsbecause a recent impact has coated part of the surface with freshlyexcavated ice. Trojans (911) Agamemnon, (617) Patroclus, (1143)Odysseus, and (2797) Teucer were also observed. These objects have beenindependently reported to show possible weak absorptions at 1.7 and 2.3?m, respectively. If real, the latter features may be due to organicmaterials present on the surfaces. However, all five targets appearspectrally featureless, even in our highest signal-to-noise ratio data.Simple models consisting of mixtures of water ice and a spectrallyfeatureless material were used to quantify the limits to surface ice.
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| Takýmyýldýz: | Yay |
| Sað Açýklýk: | 19h26m24.43s |
| Yükselim: | -38°14'04.1" |
| Görünürdeki Parlaklýk: | 9.345 |
| özdevim Sað Açýklýk: | 54.2 |
| özdevim Yükselim: | -31.3 |
| B-T magnitude: | 10.111 |
| V-T magnitude: | 9.409 |
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