M3 Goals		Science Objectives		Approach		Measurement Requriements		Baseline Return		Results
GEOLOGIC EVOLUTION
Crust		Characterize lunar highland rocks in context of geologic processes		Resolve diagnostic near-infrared mineral absorption bands of primary highland rocks.		Reflectance of surface 0.7 to 2.6 microns at <200 m spatial and <30 nm spectral resolution		Global crustal mineralogy @ 140 m/pixel; targeted areas at 70 m/pixel		Geologic processes of crustal evolution constrained
Basalts		Identify and characterize the diversity of lunar volcanism		Resolve diagnostic mineral absorption bands of basalts and estimate TiO2 of mare soils.		Reflectance of surface 0.43 to 2.6 microns at <200m and < 30 nm spectral resolution		Global basalt mineralogy @ 140 m/pixel; targeted areas at 70 m/pixel		Basaltic volcanism (mantle source) constrained in time and space
Volatiles		Identify and map the presence of hydrous phases		Detect trace amounts (of H2O and OH) from diagnostic features near 3 microns		Reflectance of surface 2.6 to 3 microns @ 50 nm resolution		Volatile assessment @ <280 m/pixel		Recent comet activity and volatile deposits identified (if present)
Fresh Craters		Evaluate the recent impact flux at 1 AU		Map the frequency of recent impactors by identifying fresh craters <0.5 km.		Reflectance of surface 400-2500 nm; global coverage at ~<200m		Global maps of soil maturity index at 140 m/pixel.		Potential hazard of 50 m NEOs at 1 AU is assessed
Unknown		Identify areas of rare or unseen lunar materials		Resolve diagnostic mineral absorption bands and compare with known species.		Reflectance of surface 0.5 to 2.6 microns at < 200 m spatial and 30 nm spectral resolution		Global mineralogy assessment @ 140 m/pixel; targeted areas at 70 m/pixel		New planetary processes and products identified; resource potential evaluated.
RESOURCES
Polar		Determine if polar H is H2O		Detect trace amounts of H2O and OH (if present) from diagnostic features near 3 microns.		Reflectance of surface 2.6 to 3 microns @ 50 nm resolution. [light source is scattered radiation from rim]		Repeated polar measurement of 3 µm feature constrains OH, H2O presence		Hydrous phases (if present) detected unambiguosly.
Local		Identify and map areas with diverse “feedstock” available		Map the composition across potential landing sites at high spatial resolution.		Reflectance of surface 0.43 to 2.6 microns at <100m spatial and 10 nm spectral resoultion		Compositon of regions of interst mapped 70 m/pixel		Optimum areas for surface “sorties” identified.

The Moon is the smallest of the rocky worlds that populate the inner solar system. Interesting in its own right as our nearest celestial neighbor, the Moon can also shed light on the development of Earth and the other terrestrial planets. Comparing the Moon to the bigger planets can help us understand the processes that shaped all of them.

Like Earth and its neighbors, the Moon underwent differentiation (separation into layers of crust, mantle, and core) early in its formation history and then experienced volcanic processes which partially recoated its surface. But unlike the more dynamic Venus, Earth and Mars, the Moon stopped at that point. Undisturbed by plate tectonics, flowing water or weathering, its surface preserves a record of those early stages of planetary development. Also preserved are records of the meteorite impacts that the Moon -- and presumably all planets in the inner solar system -- endured over the last 4 billion years.

Conveniently close and conducive to study, the Moon is probably the only planetary body we can go to with relative ease for a comprehensive analysis of how it was put together. For planetary scientists, it is a treasure trove of historical information available nowhere else. M³ will provide one of the most important keys to that treasure.

Mineralogy records the geologic character and evolution of a planet, and M³ will characterize lunar mineralogy in a spatial context, drawing relationships between visible landforms and their mineral composition. The instrument will provide scientists their first opportunity to study the Moon's surface at high spatial and spectral resolution, making spectroscopic measurements of lunar minerals in the visible and near-infrared regions of the electromagnetic spectrum, while simultaneously mapping the distribution of these materials across the surface. This information will greatly expand our understanding of the Moon and the inner solar system, and will provide a much-needed long-term baseline for future exploration activities.

One of the most persistent mysteries about the Moon is its origin. Scientists generally agree that the Moon formed from material that splashed into space when Earth was struck by an object the size of Mars. However, many important details about the Moon's formation and development remain unknown. Information from M³ will help to constrain competing models of the Moon's beginnings.

Rock and soil samples returned by the U.S. Apollo and Soviet Luna missions have provided information about the Moon's composition that is quite detailed, but restricted to a very limited region on the equatorial nearside. The more recent Clementine and Lunar Prospector missions supplied remote-sensing data of the entire surface, but at very low spectral and spatial resolution. M³ will provide data that build on the foundation of this earlier work, are not duplicated by other missions currently underway, fulfill an essential need in lunar exploration planning, and are of great scientific interest.

Goals & Objectives

The Moon Mineralogy Mapper's primary science goal is to characterize and map the mineral composition of the lunar surface to gain information about the Moon's geologic evolution. This broad topic has five distinct themes: