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Title:
Multi-Wavelength Radar Studies of Lunar Pyroclastic Deposits
Authors:
Carter, Lynn M.; Campbell, B. A.; Hawke, B. R.; Campbell, D. B.; Nolan, M. C.
Affiliation:
AA(Smithsonian Institution), AB(Smithsonian Institution), AC(University of Hawaii), AD(Cornell University), AE(NAIC/Arecibo Observatory)
Publication:
American Astronomical Society, DPS meeting #40, #9.03; Bulletin of the American Astronomical Society, Vol. 40, p.400
Publication Date:
09/2008
Origin:
AAS
Bibliographic Code:
2008DPS....40.0903C

Abstract

Lunar pyroclastic deposits were formed early in the Moon's history and are comprised of fine-grained, glassy materials. These low-albedo features are typically associated with mare boundaries, sites of mare volcanism, and fractures in and around impact craters. Optical, ultraviolet and infrared data have been used to map the locations of over one hundred pyroclastic deposits and to study their compositional differences (e.g. Gaddis et al., Icarus, 161, 262, 2003; Weitz et al., JGR, 103, 22725, 1998). We use multi-wavelength radar observations to study the distribution, depth and embedded rock abundance of these deposits. Data were acquired at S-band (12.6 cm wavelength) and P-band (70 cm wavelength) using Arecibo Observatory and the Green Bank Telescope in a bistatic configuration. The P-band images have resolutions of 150 m/pixel; S-band images have resolutions between 20 and 80 m/pixel. Pyroclastic deposits appear dark to the radar at both observed wavelengths because they are smooth, easily penetrable by radar waves, and generally contain few embedded blocks. At S-band wavelengths, changes in radar reflectivity across some of the pyroclastic deposits highlight areas with increased rock abundance. Radar circular polarization ratio maps can be used to identify fine-grained deposits in cases where optical or near-infrared data are ambiguous about the presence of pyroclastics. In some cases, data from multiple radar wavelengths (including archival 3.8 cm wavelength data) can place constraints on the deposit depth. We will present results for pyroclastic deposits surrounding Mare Serenitatis, including Sulpicius Gallus, Rima Menelaus, and Taurus-Littrow, as well as new polarimetry of the Aristarchus Plateau that compliments work done by Campbell et al. (2008, Geology, 36, 135). The S-band data are part of a larger study to map the entire lunar nearside at 80 m/pixel resolution.
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