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Analysis of Apollo Samples with the Multispectral Microscopic Imager (MMI)
Jorge I. Nuñez, Arizona State University Jack D. Farmer, Arizona State University R. Glenn Sellar, NASA Jet Propulsion Laboratory Carlton C. Allen, NASA Johnson Space Center
LEAG November 18, 2009
Microscopic Imaging is an Essential Tool for In-Situ Planetary Science
• Microspatial relationship between mineral grains and cements provides essential information for inferring primary (depositional) and secondary (diagenetic) processes
• Essential for assessing petrogenesis in the field and supports real-time, hypothesis-driven exploration
• Microscopic Imagers (MI) on the Mars Exploration Rovers • Robotic Arm Camera (RAC) and MECA on Phoenix • Mars Hand-Lens Imager (MAHLI) on Mars Science Laboratory
• Helps address goals of NRC’s Scientific Context for the Exploration of the Moon and LEAG’s Lunar Exploration Roadmap:
– Rock/soil microtextures – Rock/soil mineralogy
2009 11 18 Multispectral Microscopic Imager Nuñez et al LEAG 2009
Multispectral Microscopic Imager
• InGaAs camera – extends spectral range to
0.45 to 1.75 µm – FOV: 40 x 32 mm – Resolution: 62.5 µm/pixel
• Multiwavelength LED Illuminator – 21 wavelengths – minimizes spectral artifacts – No moving parts
2009 11 18 Multispectral Microscopic Imager Nuñez et al LEAG 2009
Multispectral Microscopic Imager
• Field-portable – battery powered – complete system 18 kg including
backpack
• Each pixel composed of VNIR spectrum
• Mineralogy within a microtextural framework: – Support in-situ rover-based analysis
of rocks and soils – Guide sub-sampling of materials for
return to Earth – Support astronaut EVA investigation
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MMI at JSC
• Initial test at JSC in May 2009
• Imaged: – 18 rocks and 4 soils – Every Apollo mission – Span full compositional range
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Apollo 15 Sample 15459 Glass-matrix Regolith Breccia
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Source: Lunar Sample Compendium
Apollo 15 Sample 15459,53
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Natural-color (463, 522, 641 nm) False-color (522, 908,1430 nm) Ratio (463/741,741/970,741/463)
Nuñez et al LEAG 2009
Ratio (1660/1050,1290/908,970/1290)
Spectral end-member map
Apollo 15 Sample 15555 Olivine-normative Basalt
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Source: Lunar Sample Compendium
Apollo 15 Sample 15555,62
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Natural-color (463, 522, 641 nm) False-color (522, 908,1430 nm) Ratio (463/741,741/970,741/463)
Nuñez et al LEAG 2009
Ratio (1660/1050,1290/908,970/1290)
Spectral end-member map
Apollo 16 Sample 60025 Ferroan Anorthosite
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Source: Lunar Sample Compendium
Apollo 16 Sample 60025,174
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Natural-color (463, 522, 641 nm) False-color (522, 908,1430 nm) Ratio (463/741,741/970,741/463)
Nuñez et al LEAG 2009
Ratio (1660/1050,1290/908,970/1290)
Spectral end-member map
Apollo 14 Sample 14321 Clast-rich, Crystalline Matrix Breccia
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Source: Lunar Sample Compendium
Apollo 14 Sample 14321,88
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Natural-color (463, 522, 641 nm) False-color (522, 908,1430 nm) Ratio (463/741,741/970,741/463)
Nuñez et al LEAG 2009
Ratio (1660/1050,1290/908,970/1290)
Spectral end-member map
Intermediate Capabilities
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Current in-situ capabilities
MMI
• Multispectral 0.4 – 1.7 µm • Some mineralogy
• Low mass • Low power • No moving parts • Sample unprepared or ground in place (e.g. MER RAT)
Not currently feasible in-situ
Hand lens • E.g. MI, RAC, MAHLI
• Very limited mineralogy
Petrographic microscope • Definitive mineralogy
• Requires extensive sample preparation
Mast-mounted cameras • E.g. MER Pancam, SSI • Multispectral 0.4- 1.0 µm
• Very limited mineralogy
Imaging spectrometers on orbiters • Hyperspectral 0.4 – 4.0 µm • E.g. OMEGA, CRISM, M3
• Substantial mineralogy
• Too massive for arm-mounted applications
Nuñez et al LEAG 2009
Optimization Within the Trade Space
2009 11 18 Multispectral Microscopic Imager
MER MI Phoenix RAC MSL MAHLI MMI M3 on Chandrayaan-1
Spectral range 0.45 – 0.7 µm 0.4 – 0.7 µm 0.4 – 0.7 µm (+ fluorescence)
0.47 – 1.75 µm 0.43 – 3.0 µm
Spectral bands 2 (closely spaced)
3 4 21 258
Mineralogical capability
none; no mineral classes identified
visible color only; few mineral classes
identified
visible color only; few mineral classes
identified
identify selected mineral classes, especially Fe-
bearing phases
identify broad range of mineral classes
Reliability no moving parts no moving parts no moving parts no moving parts scan mechanism would be required for lander/rover
Cooling not required not required not required not required detector cooled to 165 K
Mass 0.3 kg 0.4 kg 0.6 kg ~ 0.6 kg (flight version)
> 8.0 kg
Cost few $ M few $ M few $ M few $ M > $ 20 M
The MMI approach is optimal, providing substantial advances in microimaging capabilities relative to current technologies, while retaining the same low-mass (< 1 kg), low-cost (few $M), and high-reliability (no moving parts) of microimagers previously proposed for flight. Advances achieved with the MMI are accomplished within size, resource, and cost limitations for accommodation on a broad range of planetary surface missions.
Nuñez et al LEAG 2009
Summary
• The MMI produces multispectral images of rock and soil surfaces where each pixel is composed of a VNIR spectrum
• Enables the identification of lunar-relevant minerals within a microtextural framework, enabling field-based interpretations of petrogenesis
• Improves upon the capabilities of current and planned microimagers such as Phoenix’ RAC and MSL’s MAHLI by increasing the number of spectral bands and extending into the infrared
• MMI design has low mass (< 1kg), low cost, and high reliability (no moving parts) essential for arm-mounted instrument on a robotic rover or hand-held instrument for astronaut EVAs
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Acknowledgements
The research described in this paper was carried out at Arizona State University, the Jet Propulsion Laboratory, California Institute of Technology and NASA’s Johnson Space Center, under a contract with the National Aeronautics and Space Administration.
Charles Meyer, Andrea Mosie, Carol Schwarz, and Terry Parker at JSC for assistance with handling of the lunar samples, and Daniel Winterhalter at JPL for enabling the JPL/JSC initiative.
NASA Earth and Space Science Fellowship (NESSF) Program Clive Neal and LEAG for travel grant
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Questions?
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