51st Lunar and Planetary Science Conference (2020) 1357.pdf A MARTIAN METEORITE SPECTRAL LIBRARY BASED ON IN SITU PYROXENE AND BULK MARTIAN METEORITE SPECTRA. K. J. Orr1, L. V. Forman1, G. K. Benedix1, M. J. Hackett2 and V. E. Hamilton3. 1Space Science and Technology Centre (SSTC), School of Earth and Planetary Sciences, Curtin Uni- versity, Perth, Western Australia, Australia (
[email protected]), 2School of Molecular and Life Sciences, Curtin University, Perth, Western Australia, Australia, 3Southwest Research Institute, 1050 Walnut St. #300, Boulder, CO 80302 USA. Introduction: Thermal infrared spectrometers have tions using four energy dispersive x-ray (EDS) detec- been on board every major space mission to Mars. The tors which allows phase, back-scattered electron Thermal Emission Spectrometer (TES) and the Ther- (BSE) and element x-rays maps to be collected simul- mal Emission Imaging System (THEMIS), on board taneously. The analyses were run with a 70 nm spot Mars Global Survey and Mars Odyssey, respectively, size, 3 µm step size, 15 mm working distance and at have globally mapped the Martian surface in the mid- 25 kV accelerating voltage. infrared (MIR). In the MIR, spectra can be linearly Electron back-scattered diffraction (EBSD) deconvolved to determine modal mineralogy and the analyses were carried out on the sections using a MIR also allows for differentiation between various Tescan Mira3 VP-FESEM (variable pressure field silicates and their constituent phases [1]. This is emission scanning electron microscope) with an Ox- commonly done by deconvolving the Mars acquired fords Instruments Symmetry CMOS detector at the spectra using known terrestrial spectra of rocks and John de Laeter Centre in Curtin University.