Field reconnaissance geologic mapping of the Columbia Hills, Mars, based on Mars Exploration Rover Spirit and MRO HiRISE observations
Crumpler, LS and Arvidson, RE and Squyres, SW and McCoy, T and Yingst, A and Ruff, S and Farrand, W and McSween, Y and Powell, M and Ming, DW and Morris, RV and Bell III, JF and Grant, JA and Greeley, R and Des Marais, D and Schmidt, M and Cabrol, NA and Haldemann, A and Lewis, KW and Wang, AE and Schroder, C and Blaney, D and Cohen, B and Yen, A and Farmer, J and Gellert, R and Guinness, EA and Herkenhoff, KE and Johnson, JR and Klingelhofer, G and McEwen, A and Rice, JW and Rice, M and de Souza, P and Hurowitz, J, Field reconnaissance geologic mapping of the Columbia Hills, Mars, based on Mars Exploration Rover Spirit and MRO HiRISE observations, Journal of Geophysical Research-Space Physics, 116, (July 2010) EJ ISSN 0148-0227 (2010) [Refereed Article]
Chemical, mineralogic, and lithologic ground truth was acquired for the first time on Mars in terrain units mapped using orbital Mars Reconnaissance Orbiter’s High Resolution Imaging Science Experiment (MRO HiRISE) image data. Examination of several dozen outcrops shows that Mars is geologically complex at meter length scales, the record of its geologic history is well exposed, stratigraphic units may be identified and correlated across significant areas on the ground, and outcrops and geologic relationships between materials may be analyzed with techniques commonly employed in terrestrial field geology. Despite their burial during the course of Martian geologic time by widespread epiclastic materials, mobile fines, and fall deposits, the selective exhumation of deep and well‐preserved geologic units has exposed undisturbed outcrops, stratigraphic sections, and structural information much as they are preserved and exposed on Earth. A rich geologic record awaits skilled future field investigators on Mars. The correlation of ground observations and orbital images enables construction of a corresponding geologic reconnaissance map. Most of the outcrops visited are interpreted to be pyroclastic, impactite, and epiclastic deposits overlying an unexposed substrate, probably related to a modified Gusev crater central peak. Fluids have altered chemistry and mineralogy of these protoliths in degrees that vary substantially within the same map unit. Examination of the rocks exposed above and below the major unconformity between the plains lavas and the Columbia Hills directly confirms the general conclusion from remote sensing in previous studies over past years that the early history of Mars was a time of more intense deposition and modification of the surface. Although the availability of fluids and the chemical and mineral activity declined from this early period, significant later volcanism and fluid convection enabled additional, if localized, chemical activity.