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Volumn 305, Issue 5685, 2004, Pages 837-842

Initial results from the Mini-TES experiment in Gusev crater from the Spirit rover

(27)  Christensen, P R a   Ruff, S W a   Fergason, R L a   Knudson, A T a   Anwar, S a   Arvidson, R E b   Bandfield, J L a   Blaney, D L c   Budney, C c   Calvin, W M d   Glotch, T D a   Golombek, M P c   Gorelick, N a   Graff, T G a   Hamilton, V E e   Hayes, A f   Johnson, J R g   McSween Jr , H Y h   Mehall, G L a   Mehall, L K a   more..


Author keywords

[No Author keywords available]

Indexed keywords

DATA REDUCTION; MINERALOGY; PARTICLE SIZE ANALYSIS; ROCKS; SOIL MECHANICS; SPECTROMETERS; THERMODYNAMIC PROPERTIES;

EID: 3843114335     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.1100564     Document Type: Article
Times cited : (149)

References (54)
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    • The Mini-TES nominal field of view is 20 mrad at infinity. For near-field observations, the field of view is the aperture diameter (6.35 cm) plus the 20 mrad divergence from the location of the telescope to the point being observed. Targets in the arm work volume are ∼1.5 m in front of the rover, giving a total path length of ∼3 m from the Mini-TES telescope. The resulting Mini-TES field of view is ∼12 cm at the end of the rover arm.
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    • "Dust" is used throughout to indicate the fine-grained component of surface materials with similar spectral character to regional dust deposits observed by MGS TES and interpreted to be air fallout from regional and global dust storms.
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    • The mineral suite used for deconvolution included a broad range of pyroxene, feldspar, olivine, oxide, and surface dust compositions. Initial studies included carbonates and sulfates that resulted in somewhat better mathematical fits but at low (<2%) abundances of these minerals that were below detection limits. These minerals were subsequently removed from the library. The fits using only the remaining minerals give somewhat worse root mean square errors but provide a better determination of the abundances of the minerals that are reliably detected.
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    • The term martian soil is used here to denote any loose, unconsolidated materials that can be distinguished from rocks, bedrock, or strongly cohesive sediments. No implication of the presence or absence of organic materials or living matter is intended.
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    • A martian solar day has a mean period of 24 hours 39 min 35.244 s and is referred to as a sol to distinguish this from a roughly 3%-shorter solar day on Earth. A martian sidereal day, as measured with respect to the fixed stars, is 24 hours 37 min 22.663 s, as compared with 23 hours 56 min 04.0905 s for Earth. See http://www.giss.nasa.gov/tools/mars24/ for more information.
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    • The individual minerals fit to the spectra have been summed into mineral groups.
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    • The Fo (forsterite) value is the amount of FeO in the olivine, where forsterite is the Mg end-member and fayalite is the Fe end-member.
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    • note
    • We would like to express our deepest appreciation to all of the individuals at Raytheon Santa Barbara Remote Sensing led by S. Silverman, and at the Jet Propulsion Laboratory whose effort and dedication have led to the successful acquisition of Mini-TES data from the surface at Gusev Crater. Funding was provided by the MER Project Science Office.


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