DOCSLIB.ORG

A Miniaturized Chemin Xrd/Xrf for Future Mars Exploration

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
A Miniaturized Chemin Xrd/Xrf for Future Mars Exploration Ninth International Conference on Mars 2019 (LPI Contrib. No. 2089) 6230.pdf A MINIATURIZED CHEMIN XRD/XRF FOR FUTURE MARS EXPLORATION. B. Lafuente1, P. Sarrazin1, T. F. Bristow2, D. F. Blake2, M. Gailhanou3, J. Chen4, K. Thompson1, R. Walroth2, K. Zacny5, R. T. Downs6, and A. Yen7, 1SETI Institute, Mountain View, CA ([email protected]), 2Exobiology, NASA ARC, Moffett Field, CA, 3CNRS, IM2NP UMR, Marseille, France, 4Baja Technology, Tempe, AZ, 5Honeybee Robotics Spacecraft Mecha- nisms Corp., Pasadena, CA, 6Geosciences, Univ. Arizona, Tucson AZ, 7JPL, Pasadena, CA. Introduction: X-ray Diffraction (XRD) and X-ray ergy-selective detection of XRD photons in Mars’ ra- Fluorescence (XRF) analyses provide the most diag- diative environment. The CheMinX XRD geometry is nostic and complete characterization of rocks and soil based on an architecture demonstrated by hundreds of by any spacecraft-capable technique, improved upon commercial XRD instruments (Terra, commercial spin- only by sample return and analysis in terrestrial labora- off of CheMin, Fig. 1). This design resulted from a tories. In a complex sample such as a basalt, XRD can ray-tracing study of XRD geometries based on high as- definitively identify and quantify all minerals, establish pect-ratio detectors. It was found that reduced surface their individual elemental compositions and quantify area detectors can be used with no loss in throughput, the amount of the amorphous component. When cou- angular resolution or angular range, the loss in detector pled with XRF, the composition of the amorphous coverage being fully compensated for by an optimized component can be determined as well. collimator design. The MSL CheMin instrument, the first XRD instru- In its basic implementation CheMinX will provide ment flown in space, established the quantitative min- a resolution of 0.3° 2θ FWHM, slightly improved over eralogy of the Mars soil [1], characterized the first hab- CheMin’s 0.35°. A dual CCD configuration is also de- itable environment on another planet [2], and provided veloped for higher XRD resolution (0.15-0.2° 2θ the first in-situ evidence of Martian silicic volcanism FWHM based on ray tracing simulations) with no loss [3]. CheMin is now employed in the characterization of angular coverage, however at a cost in size, weight of the depositional and diagenetic environments of la- and power of the instrument. The single CCD CheM- custrine mudstones that comprise the lower strata of inX remains our focus for its ultimate miniaturization. Mt. Sharp [4]. The CheMinX design enables the use of VIS-NIR CheMin as-designed is restricted to Flagship-class spectroscopy CCD detectors in place of the large dedi- missions due to its size, mass and power. Deployment cated X-ray CCD of CheMin. As a result, the cost and of XRD/XRF on smaller (i.e., MER-class) rovers re- power requirement for CCD deep cooling are dramati- quires further miniaturization of the instrument, and cally reduced. The e2v CCD used in the Terra is also the availability of a simpler sample collection capabil- used for CheMinX, installed in an internally cooled ity than was implemented for the MSL mission. We flight-qualified package. are developing CheMinX, a new instrument benefiting from a decade of advancements in geometry design and subsystem miniaturization (Fig. 1). Fig. 2: CheMinX will use the same detector and XRD geom- etry as Terra, a commercial spin-off of CheMin. Left: Terra instrument, mass: 14.5 kg (including case, batteries and em- bedded computer), power: 75W, typical analysis time: 15 min to 1 hr, right: 2D and diffractogram XRD data. Fig. 1: The MSL CheMin instrument, 295 x260x300mm3, Sample handling: The resonant sample cells of 10.5 kg (left) vs CheMinX projected volume 2.5x smaller and CheMin are redesigned for a more compact and lower mass <5 kg (right). cost sample handling subsystem. A fixed tuning fork is CheMinX design: The XRD measurement of combined with multiple single-use cells in a CheMinX is based on the same principles as CheMin, cartridge/dispenser arrangement. A preliminary me- but uses different components and a layout optimized chanical design of CheMinX is shown in Fig. 3 com- to these components. Like in CheMin, XRD is col- pared to the CheMin sample wheel. lected by a CCD in direct illumination, critical for en- Ninth International Conference on Mars 2019 (LPI Contrib. No. 2089) 6230.pdf CheMinX as well as other planetary XRD and XRF in- struments developed by our team [5-7]. Fig. 3: Sample handling stage of CheMin with a large wheel holding a circular array of resonant sample-cell vibrators (left) versus compact design of CheMinX with single reso- nant vibrator and single-use sample cells supplied from a cartridge (right). Chemical analysis by X-ray fluorescence: For el- emental composition, CheMin used bulk sample com- Fig 4: Example of flight components under development with positions determined by a companion instrument industrial partners: A. CheMinX X-ray CCD in flight pack- (APXS). With CheMinX, the instrument provides XRF age with internal Peltier cooler (e2V); B. CCD control elec- measurement independently using an internal Silicon tronics (Baja Tech.); C. miniature microfocused X-ray tube Drift Detector (SDD) in reflection geometry. These 25kV-5W (RTW); D. X-ray tube power module with 25kV-5W spectra are quantified using Fundamental Parameters HVPS (Battel Engineering). (FP) approaches and calibrated spectra obtained from experiments conducted under the same conditions in Sample collection and delivery: CheMinX re- terrestrial laboratories. Depending on the background, quires the collection and delivery of powdered rock trace elements can be detected down to a few 10s of materials or soils. The identification of simpler sam- PPM, given sufficient collection time. pling technologies than those applied on MSL is criti- cal for the deployment of CheMinX on smaller rovers. Direct beam intensity monitoring: CheMinX has We are evaluating sample processing and delivery the capability to measure the direct beam intensity at technologies as part of this instrument development, Co Kα. This enables the measurement of sample ab- and will demonstrate CheMinX with powdering drills sorption, which varies with chemistry, compactness and arm prototypes developed at Honeybee Robotics. and thickness. Absorption inside the sample affects the overall diffracted intensity and the shape of the diffrac- Summary: Substantial reductions in mass, volume tion peaks, and is as such important for accurately and energy consumption relative to MSL CheMin are modeling the diffraction pattern for data interpretation. now possible for similar XRD performance (resolution The direct beam intensity measurement is obtained of 0.30-0.35° 2θ FWHM). An instrument with im- passively with a solid polycrystalline material (dia- proved resolution (0.2° 2θ FWHM) is also being devel- mond, silicon) positioned in the beam-stop structure to oped to provide better capabilities with complex min- diffract a single partially masked ring, proportional to eral assemblages and trace phases, at the cost of re- the transmitted beam intensity, on a lesser populated duced miniaturization. In both cases, the instrument region of the CCD. benefits from improved XRF performance by use of a Development of High TRL Components: rapid dedicated SDD placed in backscattering geometry. and cost-effective development of flight instruments CheMinX will provide quantitative mineralogy and el- requires the availability of mature technologies for the emental chemistry from drilled rocks and scooped soils critical components. High TRL subsystems are being on Mars. developed in collaboration with industrial partners: X- References: ray CCD detectors (Teledyne e2v), electronics for low [1] Science, 341, 1238932; doi:10.1126/science. noise CCD operation and embedded data processing 1238932, [2] Science, 10.1126/science.1243480. [3] (Baja Tech.), miniature microfocused X-ray tubes PNAS: doi: 10.1073/pnas.1607098113 [4] Science, (RTW), high-voltage power supplies (Battel Engineer- 356 eaah6849 DOI:10.1126/science.aah6849 [5] Wal- ing), piezoelectric actuators (Cedrat Technologies) etc roth et al, LPSC-49 #2233, [6] Blake et al, LPSC-50 (Fig. 4). These components will find applications in #1144 [7] Blake et al, LPSC-50 #1468..
Load more

Recommended publications
  • Chemical Variations in Yellowknife Bay Formation Sedimentary Rocks
    PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Chemical variations in Yellowknife Bay formation 10.1002/2014JE004681 sedimentary rocks analyzed by ChemCam Special Section: on board the Curiosity rover on Mars Results from the first 360 Sols of the Mars Science Laboratory N. Mangold1, O. Forni2, G. Dromart3, K. Stack4, R. C. Wiens5, O. Gasnault2, D. Y. Sumner6, M. Nachon1, Mission: Bradbury Landing P.-Y. Meslin2, R. B. Anderson7, B. Barraclough4, J. F. Bell III8, G. Berger2, D. L. Blaney9, J. C. Bridges10, through Yellowknife Bay F. Calef9, B. Clark11, S. M. Clegg5, A. Cousin5, L. Edgar8, K. Edgett12, B. Ehlmann4, C. Fabre13, M. Fisk14, J. Grotzinger4, S. Gupta15, K. E. Herkenhoff7, J. Hurowitz16, J. R. Johnson17, L. C. Kah18, N. Lanza19, Key Points: 2 1 20 21 12 16 2 • J. Lasue , S. Le Mouélic , R. Léveillé , E. Lewin , M. Malin , S. McLennan , S. Maurice , Fluvial sandstones analyzed by 22 22 23 19 19 24 25 ChemCam display subtle chemical N. Melikechi , A. Mezzacappa , R. Milliken , H. Newsom , A. Ollila , S. K. Rowland , V. Sautter , variations M. Schmidt26, S. Schröder2,C.d’Uston2, D. Vaniman27, and R. Williams27 • Combined analysis of chemistry and texture highlights the role of 1Laboratoire de Planétologie et Géodynamique de Nantes, CNRS, Université de Nantes, Nantes, France, 2Institut de Recherche diagenesis en Astrophysique et Planétologie, CNRS/Université de Toulouse, UPS-OMP, Toulouse, France, 3Laboratoire de Géologie de • Distinct chemistry in upper layers 4 5 suggests distinct setting and/or Lyon, Université de Lyon, Lyon, France, California Institute of Technology, Pasadena, California, USA, Los Alamos National 6 source Laboratory, Los Alamos, New Mexico, USA, Earth and Planetary Sciences, University of California, Davis, California, USA, 7Astrogeology Science Center, U.S.
    [Show full text]
  • ROVING ACROSS MARS: SEARCHING for EVIDENCE of FORMER HABITABLE ENVIRONMENTS Michael H
    PERSPECTIVE ROVING ACROSS MARS: SEARCHING FOR EVIDENCE OF FORMER HABITABLE ENVIRONMENTS Michael H. Carr* My love affair with Mars started in the late 1960s when I was appointed a member of the Mariner 9 and Viking Orbiter imaging teams. The global surveys of these two missions revealed a geological wonderland in which many of the geological processes that operate here on Earth operate also on Mars, but on a grander scale. I was subsequently involved in almost every Mars mission, both US and non- US, through the early 2000s, and wrote several books on Mars, most recently The Surface of Mars (Carr 2006). I also participated extensively in NASA’s long-range strategic planning for Mars exploration, including assessment of the merits of various techniques, such as penetrators, Mars rovers showing their evolution from 1996 to the present day. FIGURE 1 balloons, airplanes, and rovers. I am, therefore, following the results In the foreground is the tethered rover, Sojourner, launched in 1996. On the left is a model of the rovers Spirit and Opportunity, launched in 2004. from Curiosity with considerable interest. On the right is Curiosity, launched in 2011. IMAGE CREDIT: NASA/JPL-CALTECH The six papers in this issue outline some of the fi ndings of the Mars rover Curiosity, which has spent the last two years on the Martian surface looking for evidence of past habitable conditions. It is not the fi rst rover to explore Mars, but it is by far the most capable (FIG. 1). modest-sized landed vehicles. Advances in guidance enabled landing Included on the vehicle are a number of cameras, an alpha particle at more interesting and promising places, and advances in robotics led X-ray spectrometer (APXS) for contact elemental composition, a spec- to vehicles with more independent capabilities.
    [Show full text]
  • JSC-Rocknest: a Large-Scale Mojave Mars Simulant (MMS) Based Soil Simulant for In-Situ
    1 JSC-Rocknest: A large-scale Mojave Mars Simulant (MMS) based soil simulant for in-situ 2 resource utilization water-extraction studies 3 Clark, J.V.a*, Archer, P.D.b, Gruener, J.E.c, Ming, D.W.c, Tu, V.M.b, Niles, P.B.c, Mertzman, 4 S.A.d 5 a GeoControls Systems, Inc – Jacobs JETS Contract at NASA Johnson Space Center, 2101 6 NASA Pkwy, Houston, TX 77058, USA. [email protected], 281-244-7442 7 b Jacobs JETS Contract at NASA Johnson Space Center, 2101 NASA Pkwy, Houston, TX 8 77058, USA. 9 c NASA Johnson Space Center, 2101 NASA Pkwy, Houston, TX 77058, USA. 10 d Department of Earth and Environmental, Franklin & Marshall College, Lancaster, PA 17604, 11 USA. 12 *Corresponding author 13 14 15 16 17 18 19 Keywords: Simulant, Mars, In-situ resource utilization, evolved gas analysis, Rocknest 1 20 Abstract 21 The Johnson Space Center-Rocknest (JSC-RN) simulant was developed in response to a 22 need by NASA's Advanced Exploration Systems (AES) In-Situ Resource Utilization (ISRU) 23 project for a simulant to be used in component and system testing for water extraction from Mars 24 regolith. JSC-RN was designed to be chemically and mineralogically similar to material from the 25 aeolian sand shadow named Rocknest in Gale Crater, particularly the 1-3 wt.% low temperature 26 (<450 ºC) water release as measured by the Sample Analysis at Mars (SAM) instrument on the 27 Curiosity rover. Sodium perchlorate, goethite, pyrite, ferric sulfate, regular and high capacity 28 granular ferric oxide, and forsterite were added to a Mojave Mars Simulant (MMS) base in order 29 to match the mineralogy, evolved gases, and elemental chemistry of Rocknest.
    [Show full text]
  • Determining Mineralogy on Mars with the Chemin X-Ray Diffractometer the Chemin Team Logo Illustrating the Diffraction of Minerals on Mars
    Determining Mineralogy on Mars with the CheMin X-Ray Diffractometer The CheMin team logo illustrating the diffraction of minerals on Mars. Robert T. Downs1 and the MSL Science Team 1811-5209/15/0011-0045$2.50 DOI: 10.2113/gselements.11.1.45 he rover Curiosity is conducting X-ray diffraction experiments on the The mineralogy of the Martian surface of Mars using the CheMin instrument. The analyses enable surface is dominated by the phases found in basalt and its ubiquitous Tidentifi cation of the major and minor minerals, providing insight into weathering products. To date, the the conditions under which the samples were formed or altered and, in turn, major basaltic minerals identi- into past habitable environments on Mars. The CheMin instrument was devel- fied by CheMin include Mg– Fe-olivines, Mg–Fe–Ca-pyroxenes, oped over a twenty-year period, mainly through the efforts of scientists and and Na–Ca–K-feldspars, while engineers from NASA and DOE. Results from the fi rst four experiments, at the minor primary minerals include Rocknest, John Klein, Cumberland, and Windjana sites, have been received magnetite and ilmenite. CheMin and interpreted. The observed mineral assemblages are consistent with an also identifi ed secondary minerals formed during alteration of the environment hospitable to Earth-like life, if it existed on Mars. basalts, such as calcium sulfates KEYWORDS: X-ray diffraction, Mars, Gale Crater, habitable environment, CheMin, (anhydrite and bassanite), iron Curiosity rover oxides (hematite and akaganeite), pyrrhotite, clays, and quartz. These secondary minerals form and INTRODUCTION persist only in limited ranges of temperature, pressure, and The Mars rover Curiosity landed in Gale Crater on August ambient chemical conditions (i.e.
    [Show full text]
  • Chemin: a Definitive Mineralogy Instrument on the Mars Science Laboratory (Msl ’09) Rover
    Seventh International Conference on Mars 3220.pdf CHEMIN: A DEFINITIVE MINERALOGY INSTRUMENT ON THE MARS SCIENCE LABORATORY (MSL ’09) ROVER. D.F. Blake1, P. Sarrazin2, D. L. Bish3, S. J. Chipera4, D. T. Vaniman4, D. Ming5, D. Morris5 and Albert Yen6. 1NASA ARC, MS 239-4, Moffett Field, CA 94035 ([email protected]), 2 In-Xitu, Inc., 2551 Casey Ave. Ste A, Mountain View, CA 94042, 3Dept. Geological Sciences, Indiana University, Bloomington, IN 47405, 4Hydrology, Geochemistry, and Geology, Los Alamos National Laboratory, MS D469, Los Alamos, NM 87545, 5NASA Johnson Space Center, Houston, TX 77058, MS 300-315L, Pasadena, CA 91109, 6MS 183-501, Jet Propulsion Laboratory, Pasadena, CA 91109 Introduction: An important goal of the Mars Sci- a 600X600 front-illuminated frame transfer device ence Laboratory (MSL ’09) mission is the determina- having 40 !m square pixels, a deep depletion zone for tion of definitive mineralogy and chemical composi- high quantum efficiency of 7 KeV X-rays (CoK"), tion of Mars soil and rocks. CheMin is a miniature and a thin polygate structure for enhanced sensitivity X-ray diffraction (XRD) instrument that has been cho- to lower atomic number elements such as Mg. sen for the analytical laboratory of MSL [1]. CheMin uses a microfocus-source Co X-ray tube, a transmis- Table 1: Critical source and detector requirements. sion sample cell, and an energy-discriminating X-ray sensitive CCD to produce simultaneous 2-D XRD pat- Parameter Value terns and energy-dispersive X-ray histograms from powdered samples. A diagram of the instrument ge- 2! range 5-50° 2! ometry is shown in Figure 1.
    [Show full text]
  • David Vaniman, Steve Chipera, Patricia Craig Calendar Year 2018 I
    David Vaniman, Steve Chipera, Patricia Craig Calendar Year 2018 I. Report on research For calendar year 2018, focus remained on the Mars Science Laboratory (MSL) mission. Vaniman’s involvement with MSL continued in roles with two instruments, the CheMin X-ray diffraction (XRD) and X-ray florescence (XRF) instrument and, to lesser extent, the ChemCam laser-induced breakdown spectroscopy (LIBS) and remote micro-imager (RMI) instrument. Chipera and Craig are involved with the CheMin instrument. (1) Research at the MSL Gale Crater Field Site on Mars (1a) CheMin Instrument on MSL. David Vaniman is a Co-I on the CheMin instrument for Mars Science Laboratory (MSL); the PI is Tom Bristow of NASA Ames. This report also covers Steve Chipera, who is a Co-I for the CheMin instrument, and Patricia Craig, who is a Postdoctoral Research Scientist for the CheMin team. Steve Chipera works through PSI as a Senior Research Associate for the MSL mission and reports to Dave Vaniman. Patricia Craig, who is a Postdoctoral Research Scientist at PSI, also reports to Dave Vaniman. Vaniman has tactical, data analysis, and Planetary data System (PDS) reporting roles for MSL. Steve Chipera has a data analysis role and Patricia Craig has both tactical and data analysis roles for MSL. As members of the CheMin Science Team tasked with operations, Vaniman’s and Craig’s tactical participation included operations in the role of combined Payload Uplink Lead and Payload Downlink Lead (PUDL). With Dick Morris (NASA-JSC) and Mike Wilson (NASA-Ames), Vaniman completed three additional rounds of data delivery for the Planetary Data System (PDS), one on February 16, 2018 (PDS release #17), one on June 29, 2018 (PDS release #18), and one on November 2, 2018 (PDS release #19).
    [Show full text]
  • A Review of Sample Analysis at Mars-Evolved Gas Analysis Laboratory Analog Work Supporting the Presence of Perchlorates and Chlorates in Gale Crater, Mars
    minerals Review A Review of Sample Analysis at Mars-Evolved Gas Analysis Laboratory Analog Work Supporting the Presence of Perchlorates and Chlorates in Gale Crater, Mars Joanna Clark 1,* , Brad Sutter 2, P. Douglas Archer Jr. 2, Douglas Ming 3, Elizabeth Rampe 3, Amy McAdam 4, Rafael Navarro-González 5,† , Jennifer Eigenbrode 4 , Daniel Glavin 4 , Maria-Paz Zorzano 6,7 , Javier Martin-Torres 7,8, Richard Morris 3, Valerie Tu 2, S. J. Ralston 2 and Paul Mahaffy 4 1 GeoControls Systems Inc—Jacobs JETS Contract at NASA Johnson Space Center, Houston, TX 77058, USA 2 Jacobs JETS Contract at NASA Johnson Space Center, Houston, TX 77058, USA; [email protected] (B.S.); [email protected] (P.D.A.J.); [email protected] (V.T.); [email protected] (S.J.R.) 3 NASA Johnson Space Center, Houston, TX 77058, USA; [email protected] (D.M.); [email protected] (E.R.); [email protected] (R.M.) 4 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA; [email protected] (A.M.); [email protected] (J.E.); [email protected] (D.G.); [email protected] (P.M.) 5 Institito de Ciencias Nucleares, Universidad Nacional Autonoma de Mexico, Mexico City 04510, Mexico; [email protected] 6 Centro de Astrobiología (INTA-CSIC), Torrejon de Ardoz, 28850 Madrid, Spain; [email protected] 7 Department of Planetary Sciences, School of Geosciences, University of Aberdeen, Aberdeen AB24 3FX, UK; [email protected] 8 Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Armilla, 18100 Granada, Spain Citation: Clark, J.; Sutter, B.; Archer, * Correspondence: [email protected] P.D., Jr.; Ming, D.; Rampe, E.; † Deceased 28 January 2021.
    [Show full text]
  • Composition of the Rocknest Deposit, Gale Crater, Mars - PSRD | a Cosmosparks Report
    Composition of the Rocknest Deposit, Gale Crater, Mars - PSRD | A CosmoSparks report Quick Views of Big Advances Composition of the Rocknest Deposit, Gale Crater, Mars The detailed chemistry and mineralogy of a dusty, silty sand deposit at a location on Mars named Rocknest are reported in associated papers as part of a five-article series in the 27 September 2013 issue of Science that focuses on the initial results of Curiosity rover's explorations at Gale Crater. Using the rover's Alpha-Particle X-ray Spectrometer (APXS) and the CheMin powder X-ray diffraction instrument, first authors David Blake (NASA Ames Research Center) and David Bish (Indiana Univeristy) and coauthors describe the samples collected from this accumulation of wind- blown particles, also known as the Rocknest sand shadow. This self-portrait of Curiosity rover at the Rocknest sand shadow was created by mosaicing 55 MAHLI (Mars Hand Lens Imager) images from sol 84 of the mission. Dark scoop marks (numbered) are visible in the lower left corner of the image. Samples collected from the trenches were sieved to less than 150µm-size, with scoops 1 and 2 used to clean the sample handling and processing system. Samples from scoops 3, 4, and 5 were processed by the onboard instruments. The image is annotated with a blue mark to show the location of scoop 5, which was collected on a later sol. The Rocknest sand shadow is similar in appearance and composition to other wind-blown deposits at other locations on Mars; we know this from previous lander and orbital missions.
    [Show full text]
  • Composition of Mars, Michelle Wenz
    The Composition of Mars Michelle Wenz Curiosity Image NASA Importance of minerals . Role in transport and storage of volatiles . Ex. Water (adsorbed or structurally bound) . Control climatic behavior . Past conditions of mars . specific pressure and temperature formation conditions . Constrains formation and habitability Curiosity Rover at Mount Sharp drilling site, NASA image Missions to Mars . 44 missions to Mars (all not successful) . 21 NASA . 18 Russia . 1 ESA . 1 India . 1 Japan . 1 joint China/Russia . 1 joint ESA/Russia . First successful mission was Mariner 4 in 1964 Credit: Jason Davis / astrosaur.us, http://utprosim.com/?p=808 First Successful Mission: Mariner 4 . First image of Mars . Took 21 images . No evidence of canals . Not much can be said about composition Mariner 4, NASA image Mariner 4 first image of Mars, NASA image Viking Lander . First lander on Mars . Multispectral measurements Viking Planning, NASA image Viking Anniversary Image, NASA image Viking Lander . Measured dust particles . Believed to be global representation . Computer generated mixtures of minerals . quartz, feldspar, pyroxenes, hematite, ilmenite Toulmin III et al., 1977 Hubble Space Telescope . Better resolution than Mariner 6 and 7 . Viking limited to three bands between 450 and 590 nm . UV- near IR . Optimized for iron bearing minerals and silicates Hubble Space Telescope NASA/ESA Image featured in Astronomy Magazine Hubble Spectroscopy Results . 1994-1995 . Ferric oxide absorption band 860 nm . hematite . Pyroxene 953 nm absorption band . Looked for olivine contributions . 1042 nm band . No significant olivine contributions Hubble Space Telescope 1995, NASA Composition by Hubble . Measure of the strength of the absorption band . Ratio vs.
    [Show full text]
  • Slow Motion’ Field Test
    Lunar and Planetary Science XXXIX (2008) 1500.pdf CHEMCAM REMOTE ANALYSES AND IMAGING ON THE MARS SCIENCE LABORATORY 2007 ‘SLOW MOTION’ FIELD TEST. R.C. Wiens1, S. Clegg1, J. Barefield II1, D. Vaniman1, N. Lanza2, H. Newsom2, K. Herkenhoff3, N. Bridges4, D. Blaney4, S. Maurice5, O. Gasnault5, J. Blank6, M.D. Dyar7, R. Milliken8, J. Grotzinger8, J. Crisp4, and the ChemCam and MSL teams 1LANL (Los Alamos, NM; [email protected]), 2UNM (Albuquerque, NM), 3USGS (Flagstaff, AZ), 4JPL, Caltech (Pasadena, CA),5CESR (Toulouse, France), 6SETI (Mt. View, CA), 7Mount Holyoke College (South Hadley, MA) 8Caltech (Pasadena, CA), Introduction: Instrument teams from the Mars Science ter, multiple analyses were often done on a single rock to Laboratory (MSL) rover mission completed a blind field test check for heterogeneity. Unbeknownst to the MSL field test to rehearse both the instrumental analysis and decision mak- participants, the rover team determined which rock type was ing processes. MSL is scheduled to launch in late 2009 with representative of each of the many analysis requests and a suite of ten instrument packages. The 2007 slow motion instructed those carrying out the analyses which of several field test was the first such exercise for the MSL team. Par- archetype samples to use for a given analysis. ticipating instrument teams included ChemCam, CheMin, Analysis Description: Samples delivered to the Chem- APXS, SAM, and the cameras—MastCam, MAHLI, and Cam team were placed in a Mars chamber at LANL filled Hazcam and Navcam. Here we report on the analyses per- with ~7 Torr of CO2. The samples were analyzed at a dis- formed and the imaging simulated for the ChemCam remote tance of 4 m from a laboratory LIBS apparatus designed to sensing instruments.
    [Show full text]
  • Mars Science Laboratory XXX XX XXXX
    Exploring Mars with CuriosityChemCam and its Laser-Induced Remote Sensing for ChemistryLaser and Micro-Imaging (meeting) Mg Si Roger C Wiens Al Ba ChemCam PI Frontiers in Science Lectures Los Alamos – Albuquerque – Santa Fe – Taos (location) 3/16/2004 1 NASA (date)May, 2013 LA-UR-13-23209 Jean-Luc Lacour, CEA Mars Science Laboratory Goals • Assess Mars’ biological potential by • Searching for organic carbon compounds, • Looking for the chemical building blocks of life, • Identify biologically relevant clues. • Characterize the geology of the landing region • Investigate Mars’ past habitability (including the role of water) • Characterize the human hazards on Mars Spirit, Opportunity 2003 Sojourner 1997 MSL 2011 2 NASA/JPL-Caltech Is Mars Like Earth? • Starting 150 years ago, some astronomers thought they could see canals on Mars Schiaparelli 3 Mariners 4, 6, 7 Flyby Missions Mariner 4, 1965: Mars looks cratered and barren, like the Moon 4 NASA Mariner 9 Orbiter, 1971: Evidence of Water 5 NASA Viking Landers, 1976, Test for Life 6 NASA Biota Could Have Traveled From Earth to Mars • NASA has > 100 meteorites from Mars that fell to Earth • Mars probably has a number of meteorites from Earth – Bacteria from Earth could have traveled in these rocks NASA/JSC/Smithsonian 7 Fossilization How to Look for Life on Mars • Concentration: where does water deposit material? – Lakebeds and especially river deltas – Coal- or oil-bearing stata on Earth • Preservation : mineralization = fossils – Sedimentary rocks, especially clay- bearing Coal R. Wiens,
    [Show full text]
  • DOI: 10.1126/Science.1238937 , (2013); 341 Science Et Al. L. A
    Volatile, Isotope, and Organic Analysis of Martian Fines with the Mars Curiosity Rover L. A. Leshin et al. Science 341, (2013); DOI: 10.1126/science.1238937 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 information is current as of September 27, 2013 ): Updated information and services, including high-resolution figures, can be found in the online version of this article at: http://www.sciencemag.org/content/341/6153/1238937.full.html on September 27, 2013 Supporting Online Material can be found at: http://www.sciencemag.org/content/suppl/2013/09/25/341.6153.1238937.DC1.html http://www.sciencemag.org/content/suppl/2013/09/26/341.6153.1238937.DC2.html A list of selected additional articles on the Science Web sites related to this article can be found at: http://www.sciencemag.org/content/341/6153/1238937.full.html#related This article cites 43 articles, 9 of which can be accessed free: www.sciencemag.org http://www.sciencemag.org/content/341/6153/1238937.full.html#ref-list-1 This article has been cited by 3 articles hosted by HighWire Press; see: http://www.sciencemag.org/content/341/6153/1238937.full.html#related-urls 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.
    [Show full text]