Photometric Properties of Asteroid (2867) Steins in the Near-UV to Near-IR Spectral Range from Images Obtained with the OSIRIS Cameras on Rosetta

Details Photometric Properties of Asteroid (2867) Steins in the Near-UV to Near-IR Spectral Range from Images Obtained with the OSIRIS Cameras on Rosetta Photometric Properties of Asteroid (2867) Steins in the Near-UV to Near-IR Spectral Range from Images Obtained with the OSIRIS Cameras on Rosetta

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.5904k&link_type=abstract

American Astronomical Society, DPS meeting #41, #59.04

Astronomy and Astrophysics

Astronomy

Scientific paper

During the Rosetta flyby of Asteroid (2867) Steins on 5 September 2008 the OSIRIS cameras provided the first spatially resolved photometric observations of an E-type Asteroid. The spectral range between 245 nm and 990 nm was covered by low and medium bandwidth filters with a maximum spatial resolution of 80 m/pixel. The large phase angle coverage (0.3 - 140 degrees) was ideal for photometric studies.
The geometric albedo of Steins at 631 nm is 0.40 ± 0.01 and the G-Parameter in the Bowell system is 0.45, both are typical of E-type asteroids. The visible spectrum is slightly reddish, in agreement with ground-based observations. A sharp drop-off in reflectance is observed towards the hitherto unexplored near-UV region, consistent with Steins being composed of iron poor silicates. We explain the strong phase reddening seen in the date with the increasing contribution of multiple scattering to the reflected intensity at higher albedo at red wavelengths.
The surface of Steins is photometrically homogeneous to within a few percent. Space weathering is either unimportant on the surface or saturation has been reached everywhere.
Preliminary photometric modelling of the surface of (2867) Steins suggests that the brightness is consistent with an enstatite composition only if the surface is composed of particles larger than 100 µm.

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