Cordilleran Section - 113th Annual Meeting - 2017

Paper No. 12-7
Presentation Time: 8:30 AM-5:00 PM


WELLINGTON, Danika F., School of Earth & Space Exploration, Arizona State University, ISTB4 Rm 795, 781 E Terrace Mall, Tempe, AZ 85287, BELL III, James F., School of Earth & Space Exploration, Arizona State University, P.O. Box 871404, Tempe, AZ 85287, EHLMANN, Bethany, Division of Geological and Planetary Sciences, California Institute of Technology, MC170-25, Pasadena, CA 91125, and Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91104, FRAEMAN, Abigail A., Jet Propulsion Laboratory, California Institute of Technology, M/S 183-301, 4800 Oak Grove Drive, Pasadena, CA 91109, HORGAN, Briony H.N., Earth, Atmospheric, and Planetary Sciences Department, Purdue University, 550 Stadium Mall Drive, West Lafayette, IN 47907, JOHNSON, Jeffrey R., Applied Physics Laboratory, Johns Hopkins University, 11100 Johns Hopkins Road, MP3-E169, Laurel, MD 20723 and RICE, Melissa S., Geology Department, Western Washington University, 516 High St, Bellingham, WA 98225,

The Mastcam cameras on the Mars Science Laboratory Curiosity rover frequently acquire multiple-filter imaging observations along the Gale crater traverse that document the visible/near-infrared reflectance properties of the surface from 445-1012 nm. The most recent portion of the rover’s traverse through the Murray Formation has taken it into a region of elevated hematite abundance observed weakly from orbit [1], and now in situ by Mastcam and ChemCam passive [2,3] observations. In Mastcam filters, the presence of crystalline hematite is detected from an absorption near the camera’s 527 nm filter and a near-infrared band near the 867 nm filter, with a positive reflectance slope from 867 nm to the longest-wavelength filters at 1012 nm. From the ground, Mastcam has observed these hematite spectral features to be almost always present in recently-traversed Murray bedrock (since approximately sol 1160); however, significant variation exists from site to site and over small spatial scales. Spectral differences in the strength of the 867 to 1012 nm spectral slope, visible wavelength color (e.g., red/blue ratio), and differences in overall reflectance and peak reflectance wavelength are typical of the diversity in spectral properties that the cameras have observed. These variations suggest differences in mineral grain sizes and/or abundances of iron-bearing mineral phases. Mastcam multispectral observations are helping to document and define additional in situ measurements needed to understand the complex aqueous history within Gale crater.

[1] Fraeman et al. (2016) AGU Fall Meeting abstract P23B-2173 [2] Johnson et al. (2016) LPSC abstract #1155. [3] Johnson et al. (2017) LPSC abstract #1301.