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Title:
A High Resolution Radar Survey of the Lunar Near Side
Authors:
Campbell, Donald B.; Campbell, B. A.; Carter, L. M.; Ghent, R. R.; Nolan, M. C.; Wells, K. S.
Affiliation:
AA(Cornell Univ), AB(Smithsonian Institution), AC(Smithsonian Institution), AD(University of Toronto, Canada), AE(NAIC/Arecibo Observatory), AF(Cornell Univ)
Publication:
American Astronomical Society, DPS meeting #40, #9.02; Bulletin of the American Astronomical Society, Vol. 40, p.400
Publication Date:
09/2008
Origin:
AAS
Bibliographic Code:
2008DPS....40.0902C

Abstract

Since 2005 we have been using the Arecibo 13 cm transmitting system and the 100 m Green Bank Telescope (GBT) in a bi-static radar configuration for multi-polarization imaging of the lunar surface at resolutions as fine as 20 m. A circularly polarized wave is transmitted and the echo received in both senses of received circular polarization, allowing imaging in the full Stokes’ polarization parameters of the reflected signal. The initial objective was the South Pole region, with emphasis on high-resolution images of possible landing sites and polarimetric analysis of putative ice deposits (D. Campbell et al, 2006 Nature, 443, 835). A byproduct of this work was a method for clearly identifying secondary craters from Tycho via their circular polarization ratio signature (K. Wells et al, 2006, DPS abst). Subsequent observations have concentrated on studies of pyroclastic deposits including potentially resource-rich areas such as the Aristarchus plateau, where the radar's ability to probe the sub-surface has allowed the subsurface rock distribution to be investigated (B. Campbell et al, 2008, Geology, 36, 135; Carter et al, 2007 LPSC Conf. 38, Houston, Texas).

We have begun a systematic mapping program that will image most of the near side of the Moon in the full Stokes parameters. The initial product is a large area image of the south-polar region at 20 m resolution, with one look (see http://arecibo.tc.cornell.edu/lunarimages/default.aspx). To reduce the required observation time to an acceptable level, subsequent images will be at 80 m resolution, four looks. The results will be made available through the PDS.

We acknowledge the NASA Planetary Astronomy program for partial support of this work and NAIC and NRAO for making Arecibo and the GBT available for the observations.

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