Mapping Vesta with Adaptive Optics: the 1996 Opposition

Details Mapping Vesta with Adaptive Optics: the 1996 Opposition Mapping Vesta with Adaptive Optics: the 1996 Opposition

Sep 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996dps....28.1024d&link_type=abstract

American Astronomical Society, DPS meeting #28, #10.24; Bulletin of the American Astronomical Society, Vol. 28, p.1101

Physics

Optics

2

Scientific paper

The geometry of the 1996 opposition of Vesta was particularly favorable since its angular diameter was 0\farcs65 and more than 99% of its surface was visible. Using ground-based telescopes equipped with an adaptive optics system, we imaged Vesta at three wavelengths accross the first absorption band of pyroxene (0.7, 0.83 and 0.94 mu m). We obtained images from the 100 inch telescope at Mount-Wilson Observatory, the 3.6 m Canada-France-Hawai`i Telescope on Mauna Kea and the 1.5 m telescope at the ``Observatoire de Haute-Provence'' in France. At these wavelengths, Vesta appears to show some strong variation of albedo directly related to the impacts undergone since it was formed. The images below have been recorded 20 minutes apart on June 14, 1996 at Mount Wilson through two different narrow band filters (left: 0.7 mu m - right:0.83mu m). From this sample it appears that the shape of Vesta is extremely irregular. We can also identify some albedo features on the surface and follow their rotation. From the entire data set, it will be possible to derive the shape of the asteroid as well as the surface distribution of pyroxene and feldspar. We will also discuss the extension of this high-resolution mapping project to other main-belt asteroids and our prospects concerning the mineralogical mapping of Vesta for the next opposition of October 1997.

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