The Moon Mineralogy Mapper (M3) imaging spectrometer for lunar science: Instrument description, calibration, on‐orbit measurements, science data calibration and on‐orbit validation
Robert O. Green,Carle M. Pieters,Pantazis Mouroulis,Michael L. Eastwood,Joseph W. Boardman,T. Glavich,Peter J. Isaacson,M. Annadurai,Sebastien Besse,D. Barr,B. J. Buratti,D. Cate,A. Chatterjee,Ross A. Clark,L. C. Cheek,J. P. Combe,Deepak Dhingra,V. Essandoh,Sven Geier,J. N. Goswami,R. R. Green,V. Haemmerle,James W. Head,L. Hovland,S. Hyman,Rachel L. Klima,Rachel L. Klima,T. Koch,Georgiana Y. Kramer,A.S.K. Kumar,Kenneth Lee,S. Lundeen,Erick Malaret,T. B. McCord,S. McLaughlin,John F. Mustard,J. Nettles,Noah E. Petro,K. Plourde,C. Racho,J. Rodriquez,C. Runyon,Glenn Sellar,Charles W. Smith,H. Sobel,M. Staid,Jessica M. Sunshine,Lawrence A. Taylor,K. G. Thaisen,Stefanie Tompkins,H. Tseng,G. Vane,P. Varanasi,M. White,D. Wilson +54 more
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The NASA Discovery Moon Mineralogy Mapper imaging spectrometer was selected to pursue a wide range of science objectives requiring measurement of composition at fine spatial scales over the full lunar surface.Abstract:
[1] The NASA Discovery Moon Mineralogy Mapper imaging spectrometer was selected to pursue a wide range of science objectives requiring measurement of composition at fine spatial scales over the full lunar surface. To pursue these objectives, a broad spectral range imaging spectrometer with high uniformity and high signal-to-noise ratio capable of measuring compositionally diagnostic spectral absorption features from a wide variety of known and possible lunar materials was required. For this purpose the Moon Mineralogy Mapper imaging spectrometer was designed and developed that measures the spectral range from 430 to 3000 nm with 10 nm spectral sampling through a 24 degree field of view with 0.7 milliradian spatial sampling. The instrument has a signal-to-noise ratio of greater than 400 for the specified equatorial reference radiance and greater than 100 for the polar reference radiance. The spectral cross-track uniformity is >90% and spectral instantaneous field-of-view uniformity is >90%. The Moon Mineralogy Mapper was launched on Chandrayaan-1 on the 22nd of October. On the 18th of November 2008 the Moon Mineralogy Mapper was turned on and collected a first light data set within 24 h. During this early checkout period and throughout the mission the spacecraft thermal environment and orbital parameters varied more than expected and placed operational and data quality constraints on the measurements. On the 29th of August 2009, spacecraft communication was lost. Over the course of the flight mission 1542 downlinked data sets were acquired that provide coverage of more than 95% of the lunar surface. An end-to-end science data calibration system was developed and all measurements have been passed through this system and delivered to the Planetary Data System (PDS.NASA.GOV). An extensive effort has been undertaken by the science team to validate the Moon Mineralogy Mapper science measurements in the context of the mission objectives. A focused spectral, radiometric, spatial, and uniformity validation effort has been pursued with selected data sets including an Earth-view data set. With this effort an initial validation of the on-orbit performance of the imaging spectrometer has been achieved, including validation of the cross-track spectral uniformity and spectral instantaneous field of view uniformity. The Moon Mineralogy Mapper is the first imaging spectrometer to measure a data set of this kind at the Moon. These calibrated science measurements are being used to address the full set of science goals and objectives for this mission.read more
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Direct evidence of surface exposed water ice in the lunar polar regions
Shuai Li,Shuai Li,Paul G. Lucey,Ralph E. Milliken,Paul O. Hayne,E. A. Fisher,Jean-Pierre Williams,Dana M. Hurley,Richard C. Elphic +8 more
TL;DR: Direct and definitive evidence for surface-exposed water ice in the lunar polar regions is found and the observation of spectral features of H2O confirms that water ice is trapped and accumulates in permanently shadowed regions of the Moon and in some locations, it is exposed at the modern optical surface.
Journal ArticleDOI
An introduction to the NASA Hyperspectral InfraRed Imager (HyspIRI) mission and preparatory activities
Christine Lee,Morgan L. Cable,Simon J. Hook,Robert O. Green,Susan L. Ustin,Daniel Mandl,Elizabeth M. Middleton +6 more
TL;DR: The NASA Hyperspectral InfraRed Imager (HyspIRI) as mentioned in this paper is comprised of a visible to short-wavelength infrared (VSWIR) imaging spectrometer and a thermal infrared (TIR) multispectral imager, together with an Intelligent Payload Module (IPM) for onboard processing and rapid downlink of selected data.
Journal ArticleDOI
Magmatic volatiles (H, C, N, F, S, Cl) in the lunar mantle, crust, and regolith: Abundances, distributions, processes, and reservoirs
Francis M. McCubbin,Kathleen E. Vander Kaaden,Romain Tartèse,Rachel L. Klima,Yang Liu,J. Mortimer,Jessica Barnes,Jessica Barnes,Charles K. Shearer,Allan H. Treiman,David J. Lawrence,Stephen M. Elardo,Stephen M. Elardo,Dana M. Hurley,Jeremy W. Boyce,Mahesh Anand,Mahesh Anand +16 more
TL;DR: In this paper, the authors used the phase assemblages present in coatings on those beads to infer that the primary vapor component responsible for propelling fire-fumarolic eruptions in pyro-glass beads was used to determine the source of volatiles in the Moon.
Journal ArticleDOI
The evolution of rifting on the volcanic margin of the Pelotas Basin and the contextualization of the Paraná–Etendeka LIP in the separation of Gondwana in the South Atlantic
TL;DR: The analysis of rifting in this portion of the South Atlantic is based on seismic interpretation and on the distribution of regional linear magnetic anomalies as mentioned in this paper, which is a very different geology from the adjacent Santos, Campos and Espirito Santo Basins, which constitute examples of magma-poor passive margins.
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