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Evidence from Opportunity's Microscopic Imager for Water on Meridiani Planum K

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Evidence from Opportunity's Microscopic Imager for Water on Meridiani Planum K Evidence from Opportunity's Microscopic Imager for Water on Meridiani Planum K. E. Herkenhoff, et al. Science 306, 1727 (2004); DOI: 10.1126/science.1105286 This copy is for your personal, non-commercial use only. If you wish to distribute this article to others, you can order high-quality copies for your colleagues, clients, or customers by clicking here. Permission to republish or repurpose articles or portions of articles can be obtained by following the guidelines here. The following resources related to this article are available online at www.sciencemag.org (this infomation is current as of October 27, 2011 ): Updated information and services, including high-resolution figures, can be found in the online version of this article at: http://www.sciencemag.org/content/306/5702/1727.full.html Supporting Online Material can be found at: http://www.sciencemag.org/content/suppl/2004/11/30/306.5702.1727.DC1.html A list of selected additional articles on the Science Web sites related to this article can be on October 27, 2011 found at: http://www.sciencemag.org/content/306/5702/1727.full.html#related This article has been cited by 70 article(s) on the ISI Web of Science This article has been cited by 10 articles hosted by HighWire Press; see: http://www.sciencemag.org/content/306/5702/1727.full.html#related-urls This article appears in the following subject collections: Planetary Science www.sciencemag.org http://www.sciencemag.org/cgi/collection/planet_sci Downloaded from Science (print ISSN 0036-8075; online ISSN 1095-9203) is published weekly, except the last week in December, by the American Association for the Advancement of Science, 1200 New York Avenue NW, Washington, DC 20005. Copyright 2004 by the American Association for the Advancement of Science; all rights reserved. The title Science is a registered trademark of AAAS. O PPORTUNITY AT M ERIDIANI P LANUM S REPORT PECIAL Evidence from Opportunity’s Microscopic Imager S for Water on Meridiani Planum ECTION K. E. Herkenhoff,1* S. W. Squyres,2 R. Arvidson,3 D. S. Bass,4 J. F. Bell III,2 P. Bertelsen,5 B. L. Ehlmann,3 W. Farrand,6 L. Gaddis,1 R. Greeley,7 J. Grotzinger,8 A. G. Hayes,2 S. F. Hviid,9 J. R. Johnson,1 B. Jolliff,3 K. M. Kinch,10 A. H. Knoll,11 M. B. Madsen,5 J. N. Maki,4 S. M. McLennan,12 H. Y. McSween,13 D. W. Ming,14 J. W. Rice Jr.,7 L. Richter,15 M. Sims,16 P. H. Smith,17 L. A. Soderblom,1 N. Spanovich,17 R. Sullivan,2 S. Thompson,7 T. Wdowiak,18 C. Weitz,19 P. Whelley7 The Microscopic Imager on the Opportunity rover analyzed textures of soils and indicated where this results in very short, rocks at Meridiani Planum at a scale of 31 micrometers per pixel. The uppermost near-vertical walls in the surrounding soil millimeter of some soils is weakly cemented, whereas other soils show little (Fig. 1). Some MI observations of soils evidence of cohesion. Rock outcrops are laminated on a millimeter scale; image disturbed by the MB contact plate show mosaics of cross-stratification suggest that some sediments were deposited by apparent fractures, suggesting that cementa- flowing water. Vugs in some outcrop faces are probably molds formed by tion of surface particles has formed a crust. dissolution of relatively soluble minerals during diagenesis. Microscopic images The thickness of this crust is estimated to be support the hypothesis that hematite-rich spherules observed in outcrops and soils at least 1 mm (the penetration depth of the also formed diagenetically as concretions. MB contact plate) based on images taken after the surface was disrupted (e.g., Fig. 1). The Athena science payload on the Mars During the first 90 sols (4) of its surface Plausibly, and consistent with Alpha Particle Exploration Rover (MER) mission includes mission (5), the Opportunity rover acquired X-Ray Spectrometer (APXS) spectra of soil- the Microscopic Imager (MI), a camera and returned 870 MI images (including like deposits at the Meridiani site (11), the designed to provide views that are similar subframes) of rocks, soil/bedform targets, cementation is caused by precipitation of _ on October 27, 2011 to that seen through a geologist s hand lens and the martian sky (for calibration). Tracks various salts (e.g., Cl- and SO4-bearing) that (1, 2). MI data are acquired in order to place and trenches created by the rover wheels bridge soil particles. Salts in the dust (unre- other MER instrument data in context and to were also imaged (6), as were the filter and solved by the MI) may dissolve and migrate aid in petrologic and geologic interpretations capture magnets on the front of the rover (7). into voids between soil particles in thin films of rocks and soils on Mars. The MI on MI observations of soil-like materials of water (12) adsorbed onto soil particles. Opportunity is essentially identical to the MI (8) within Eagle crater (9) and on the sur- Thin liquid films may occur in soils when the on Spirit and is used in a similar manner (3). rounding plains have been used to assess spin axis obliquity and atmospheric relative cohesion and cementation of very fine- humidity are high enough to cause precipita- G 1U.S. Geological Survey Astrogeology Team, Flagstaff, grained ( 125 mm) material, based on soil tion or condensation of water. During warm- AZ 86001, USA. 2Department of Astronomy, Space morphology after disturbances caused by ing events, salts precipitate on soil particles as www.sciencemag.org Sciences Building, Cornell University, Ithaca, NY the rover wheels and by the MPssbauer thin liquid films evaporate (13), weakly 3 14853, USA. Department of Earth and Space spectrometer(MB)contactplate(10). cementing the upper soil surface. Sciences, Washington University, St. Louis, MO 63130, USA. 4Jet Propulsion Laboratory, California Granules on the surface typically are In many places, Meridiani soils contain a Institute of Technology, Pasadena, CA 91109, USA. pressed into the underlying very fine sand major, distinctive component in the form of 5Center for Planetary Science, Danish Space Research by MB contact; cohesion between grains is 0.6- to 6-mm-diameter spherules (14). These Institute and Niels Bohr Institute for Astronomy, Physics and Geophysics, University of Copenhagen, Denmark. 6Space Science Institute, Boulder, CO Downloaded from 80301, USA. 7Department of Geological Sciences, Fig. 1. False-color merge of MI Arizona State University, Tempe, AZ 85287, USA. image of target Munter 8Department of Earth, Atmospheric and Planetary (1M133692453), taken on sol Sciences, Massachusetts Institute of Technology, 62, with Pancam multispectral Cambridge, MA 02139, USA. 9Max Planck Institut data (effective wavelengths of fu¨r Aeronomie, Katlenburg-Lindau, D-37191, Ger- 602, 535, and 483 nm). The MI many. 10Institute of Physics and Astronomy, Aarhus image was acquired after MB University, Aarhus, Denmark. 11Department of Or- contact, when the target was in ganismic and Evolutionary Biology, Harvard Univer- complete shadow. The area sity, Cambridge, MA 02138, USA. 12State University shown is 3 cm across. of New York, Department of Geosciences, Stony Brook, NY 11794, USA. 13Department of Earth and Planetary Sciences, University of Tennessee, Knox- ville, TN 37996, USA. 14Astromaterials Research and Exploration Science Office, NASA Johnson Space Center, Houston, TX 77058, USA. 15DLR Institut fur Raumsimulation, Linder Hoehe, Koln, Germany. 16NASA Ames Research Center, Moffett Field, CA 94035, USA. 17Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA. 18Department of Physics, University of Alabama, Birmingham, AL 35294, USA. 19Planetary Science Institute, Tucson, AZ 85719, USA. *To whom correspondence should be addressed. E-mail: [email protected] www.sciencemag.org SCIENCE VOL 306 3 DECEMBER 2004 1727 OOPPORTUNITYPPORTUNITY AT ATMMERIDIANIERIDIANIPPLANUMLANUM spherules, interpreted to be hematitic con- cretions (5), are also found as a relatively ECTION resistant component of the outcrops exposed S in the walls of Eagle and Fram craters. These observations indicate that the spherules are more resistant to physical and/or chemical erosion than the supporting outcrop matrix. PECIAL Two other classes of coarse particles are S usually present: (i) subangular, irregular particles 1.5 to 5.0 mm in maximum dimen- sion, some with submillimeter circular voids; and (ii) rounded particles 0.5 to 2.0 mm in Fig. 2. Part of merge of five MI images of diameter that are not derived from the outcrop feature McKittrick (1M130672440 to 1M130672724), taken on sol 28. Illumination is spherules or spherule fragments. The ir- from the top, and the area shown is 2.8 cm regular particles are probably vesicular across. Concentric banding in the shaded face Fig. 3. Part of MI image 1M132444583 of tar- basalt fragments, based on their morphology of a broken spherule is indicated by the arrow. get Tripleberry in the Berry Bowl, taken on sol and color (14). The rounded particles are Vugs cut across subhorizontal bedding and are 48 when the target was in full shadow. The area shown is 1.4 cm across. often found, along with spherule fragments, partly filled by dark, very fine sand grains. within or emerging from a matrix of fine- grained sand and armor ripple bedforms (6). Meridiani have recently been moved by form mm-scale laminations; (ii) fine-grained MI images of the soil taken soon after winds, causing dust removal from grain and coarser crystalline textures of subse- egress show a soil dominated by dark, very surfaces. MI images (Fig. 1) suggest that at quently precipitated cements and areas of fine-grained (G125 mm) particles. Closer to the surface the fine-grained material is well recrystallization; (iii) centimeter-size vugs the outcrop, soils contain a greater propor- sorted with a mean grain size in the range of that record the early diagenetic growth and tional abundance of spherules.
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