Analysis of Apollo Samples with the Multispectral ... PM... · 2009 11 18 Multispectral Microscopic Imager Nuñez et al LEAG 2009 . Multispectral Microscopic Imager ... M. S. Robinson,

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


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


MMI at JSC

•  Initial test at JSC in May 2009

•  Imaged: –  18 rocks and 4 soils –  Every Apollo mission –  Span full compositional range


Apollo 15 Sample 15459 Glass-matrix Regolith Breccia


Source: Lunar Sample Compendium

Apollo 15 Sample 15459,53

2009 11 18 Multispectral Microscopic Imager

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







Ratio (1660/1050,1290/908,970/1290)


Apollo 16 Sample 60025 Ferroan Anorthosite







Ratio (1660/1050,1290/908,970/1290)


Apollo 14 Sample 14321 Clast-rich, Crystalline Matrix Breccia







Ratio (1660/1050,1290/908,970/1290)


Intermediate Capabilities


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


Optimization Within the Trade Space


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.


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


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


Questions?


References

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Analysis of Apollo Samples with the Multispectral ... PM... · 2009 11 18 Multispectral Microscopic Imager Nuñez et al LEAG 2009 . Multispectral Microscopic Imager ... M. S. Robinson,