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Reflectance Spectra Diversity of Silica-Rich Materials: Sensitivity to Environment and Implications for Detections on MarsHydrated silica-rich materials have recently been discovered on the surface of Mars by the Mars Exploration Rover (MER) Spirit, the Mars Reconnaissance Orbiter (MRO) Compact Reconnaissance Imaging Spectrometer for Mars (CRISM), and the Mars Express Observatoire pour la Mineralogie, l'Eau, les Glaces, et l'Activite'(OMEGA) in several locations. Having been interpreted as hydrothermal deposits and aqueous alteration products, these materials have important implications for the history of water on the martian surface. Spectral detections of these materials in visible to near infrared (Vis NIR) wavelengths have been based on a H2O absorption feature in the 934-1009 nm region seen with Spirit s Pancam instrument, and on SiOH absorption features in the 2.21-2.26 micron range seen with CRISM. Our work aims to determine how the spectral reflectance properties of silica-rich materials in Vis NIR wavelengths vary as a function of environmental conditions and formation. Here we present laboratory reflectance spectra of a diverse suite of silica-rich materials (chert, opal, quartz, natural sinters and synthetic silica) under a range of grain sizes and temperature, pressure, and humidity conditions. We find that the H2O content and form of H2O/OH present in silica-rich materials can have significant effects on their Vis NIR spectra. Our main findings are that the position of the approx.1.4 microns OH feature and the symmetry of the approx.1.9 microns feature can be used to discern between various forms of silica-rich materials, and that the ratio of the approx.2.2 microns (SiOH) and approx.1.9 microns (H2O) band depths can aid in distinguishing between silica phases (opal-A vs. opal-CT) and formation conditions (low vs. high temperature). In a case study of hydrated silica outcrops in Valles Marineris, we show that careful application of a modified version of these spectral parameters to orbital near-infrared spectra (e.g., from CRISM and OMEGA) can aid in characterizing the compositional diversity of silica-bearing deposits on Mars. We also discuss how these results can aid in the interpretation of silica detections on Mars made by the MER Panoramic Camera (Pancam) and Mars Science Laboratory (MSL) Mast-mounted Camera (Mastcam) instruments.
Document ID
20130013618
Document Type
Reprint (Version printed in journal)
Authors
Rice, M. S. (California Inst. of Tech. Pasadena, CA, United States)
Cloutis, E. A. (Winnipeg Univ. Manitoba, Canada)
Bell, J. F., III (Arizona State Univ. Tempe, AZ, United States)
Bish, D. L. (Indiana Univ. Bloomington, IN, United States)
Horgan, B. H. (Arizona State Univ. Tempe, AZ, United States)
Mertzman, S. A. (Franklin and Marshall Coll. Lancaster, PA, United States)
Craig, M. A. (University of Western Ontario London, Ontario, Canada)
Renault, R. W. (Saskatchewan Univ. Saskatoon, Saskatchewan, Canada)
Gautason, B. (Iceland Geodetic Survey Reykjavik, Iceland)
Mountain, B. (GNS Science Taupo, New Zealand)
Date Acquired
August 27, 2013
Publication Date
March 1, 2013
Publication Information
Publication: Icarus
Volume: 223
Issue: 1
Subject Category
Lunar and Planetary Science and Exploration
Funding Number(s)
CONTRACT_GRANT: NNX11AE66G
Distribution Limits
Public
Copyright
Other