DOCSLIB.ORG

The Moon Mineralogy Mapper (M3) on Chandrayaan-1

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The Moon Mineralogy Mapper (M3) on Chandrayaan-1 Lunar Reconnaissance Orbiter Science Targeting Meeting (2009) 6002.pdf CHARACTERIZATION OF LUNAR MINERALOGY: THE MOON MINERALOGY MAPPER (M3) ON CHANDRAYAAN-1. C. M. Pieters1, J. Boardman2, B. Buratti3, R. Clark4, J-P Combe5, R. Green3, J. W. Head III1, M. Hicks3, P. Isaacson1, R. Klima1, G. Kramer5, S. Lundeen3, E. Malaret7, T. B. McCord5, J. Mustard1, J. Nettles1, N. Petro8, C. Runyon9, M. Staid10, J. Sunshine11, L. Taylor12, S. Tompkins13, P. Varanasi3 1Dept. Geological Sci- ences, Brown University, Providence, RI 02912 ([email protected]), 2AIG, 3JPL, 4USGS Denver, 5Bear Fight Center, WA, 6ISRO-PRL, 7ACT, 8NASA Goddard, 9College of Charleston, 10PSI, 11Univ. MD, 12Univ. Tenn., 13DARPA. The Moon Mineralogy Mapper (M3, pronounced “m- M3 Measurement Modes cube”) is a state-of-the-art high spectral resolution imag- All M3 Spectroscopic data (from 100 km orbit): ing spectrometer that is orbiting the Moon on 40 km FOV, contiguous orbits Chandrayaan-1, the Indian Space Research Organization 0.70 to 3.0 µm [0.43 to 3.0 µm achieved] (ISRO) mission to the Moon. M3 is one of several for- Targeted Mode: Full Resolution Science targets eign instruments chosen by ISRO to be flown on 70 m/pixel spatial (600 pixel crosstrack) Chandrayaan-1 to complement the strong ISRO payload. 10 nm spectral [260 bands] M3 is a NASA Discovery Mission of Opportunity se- Global Mode: Lower Resolution Global Coverage lected through peer-review as part of the SMD 140 m/pixel spatial (300 pixel crosstrack) Discovery Program. 20 & 40 nm selected (85 bands, averaging) The type and composition of minerals that comprise a planetary surface are a direct result of the initial compo- In February 2009, Chandrayaan-1 completed its pri- sition and later thermal and physical processing. Lunar mary commissioning phase. During this initial period M3 mineralogy seen today is a direct record of the early evo- operated principally in Global Mode. The low resolution lution of the lunar crust and subsequent geologic Global Mode M3 coverage achieved for the nearside is processes. Specifically, the distribution and concentra- shown in Figure 1. A closer view of one band of several tion of individual minerals or groups of minerals is neighboring M3 swaths is shown in Figure 2. Both im- closely tied to magma ocean products, lenses of intruded ages are compressed to meet abstract requirements. Pre- or remelted plutons, basaltic volcanism and fire- calibration assessment of these data (over one billion fountaining, and any process (e.g. cratering) that might spectra) indicates they are of excellent quality, meeting redistribute or transform primary and secondary lunar all instrument requirements for science. Early results are crustal materials. The primary science goal of M3 is to presented in [1, 2]; a descriptive overview of M3 is found characterize and map lunar surface mineralogy in the in [3] along with other Chandrayaan-1 instruments. context of its geologic evolution, and the primary explo- At least three full optical imaging periods are planned ration goal is to assess and map lunar mineral resources over the next two years. For M3, we have two prime at high spatial resolution to support planning for future, measurement periods in each imaging period. Our plans targeted missions. are to complete M3 coverage for the entire Moon using M3 is first and foremost a near-infrared spectrometer the 140 m Global mode and to then acquire optimum full designed to accurately measure diagnostic mineral ab- resolution data (Target mode) for the highest priority sorption features. To meet the above science and science targets. exploration goals, M3 acquires spectra in image format (all spectral channels co-registered to < 0.1 pixel). M3 References: 1) Pieters et al., 2009, LPSC40 #2052 2) operates in two measurement modes as summarized be- Green et al., 2009, LPSC40 #2307. 3) Pieters et al., low. 2009, Current Science, Vol. 96, No. 4. Lunar Reconnaissance Orbiter Science Targeting Meeting (2009) 6002.pdf Figure 1. Overview of M3 Global mode coverage acquired in February at the end of commissioning phase of the first optical period of Chandrayaan-1. Each M3 data swath is 40 km wide. Shown is one channel of M3 data. No photometric corrections have been made, but since each swath is scaled independently, swath boundaries are evident. (Background is Clementine ) Figure 2. Subset of Fig. 1 containing Kepler crater. This M3 image includes 8 orbits of data. A M3spectrum exists for each pixel. .
Load more

Recommended publications
  • 1 Dr. Shuai Li Hawaii Institute of Geophysics and Planetology
    Dr. Shuai Li Hawaii Institute of Geophysics and Planetology, University of Hawaii at Manoa [email protected] 1(401) 632-1933 Areas of Research Interest Spectroscopy (visible to mid-infrared); water formation, retention, migration, and sequestration on rocky bodies; remote sensing of planetary surface compositions; planetary petrology; surface processes on the Moon, particularly in the polar regions; lunar magnetic anomalies; chaos terrains on Europa. Research Tools / Skills Radiative transfer theories/modeling for reflectance spectroscopy; diffusion modeling for heat and elements; empirical modeling of remote sensing data; applications of artificial intelligence (AI) in remote sensing; complex processing of large orbital remote sensing data (>TB). Programing languages (expert): C/C++, MATLAB, MFC, C++ Builder, IDL. Working Experience Assistant Researcher, Hawaii Institute of Geophysics and Planetology, University of Hawaii at Manoa 2020 - present Postdoctoral Research Associate, Hawaii Institute of Geophysics and Planetology, University of Hawaii at Manoa 2017 – 2020 Postdoctoral Research Associate, Department of Earth, Environmental and Planetary Sciences, Brown University (Providence, RI) 2016 – 2017 Research Assistant, Department of Earth, Environmental and Planetary Sciences, Brown University (Providence, RI) 2012 – 2016 Education Brown University (Providence, RI) 2011 - 2016 Doctor of Philosophy; advisor: Prof. Ralph E. Milliken Indiana University - Purdue University Indianapolis (Indianapolis, IN). 2009 - 2011 M.S. in Geology Institute of Remote Sensing Applications, CAS (Beijing, China) 2007 - 2009 M.S. in Environmental Sciences Nanjing University (Nanjing, China) 2003 - 2007 B.S. in Geology Honors and Awards 2017, Bernard Ray Hawke Next Lunar Generation Career Development Awards, NASA LEAG 2013, NASA Group Achievement Award, MSL Science Office Development and Operations Team 2009, Arthur Mirsky Fellowship, Indiana University – Purdue University Indianapolis 1 Selected Peer-Reviewed Publications Planetary Sciences 1.
    [Show full text]
  • Water Found on the Moon
    Water Found on the Moon • Analysis of lunar rocks collected by Apollo astronauts did not reveal the presence of water on the Moon • Four spacecraft recently reported small amounts of H2O and/or OH at the Moon: • India’s Chandrayaan mission • NASA’s Cassini mission • NASA’s EPOXI mission • NASA’s LCROSS mission The first three measured the top few mm of the lunar surface. LCROSS measured plumes of lunar gas and soil ejected when a part of the spacecraft was crashed into a crater. This false-color map created from data taken by NASA’s Moon Mineralogy Mapper (M3) on • How much water? Approximately 1 ton of Chandrayaan is shaded blue where trace lunar regolith will yield 1 liter of water. amounts of water (H2O) and hydroxyl (OH) lie in the top few mm of the surface. Discoveries in Planetary Science http://dps.aas.org/education/dpsdisc/ How was Water Detected? • Lunar soil emits infrared model with thermal thermal radiation. The radiation only amount of emitted light at each wavelength varies model with thermal smoothly according to the radiation and Moon’s temperature. Intensity absorption by molecules • H2O or OH molecules in the soil absorb some of the radiation, but only at specific wavelengths Wavelengths where water absorbs light • All four infrared spectrographs Intensity measure a deficit of thermal radiation at those wavelengths, implying water is present An infrared spectrum measured by LCROSS (black data points) compared to models (red line) Discoveries in Planetary Science http://dps.aas.org/education/dpsdisc/ The Big Picture • Lunar water may come from ‘solar wind’ hydrogen striking the surface, combining with oxygen in the soil.
    [Show full text]
  • Exploring Space Through Sample Return Missions: How, Where, and What Do We Do with the Rocks?
    Exploring Space through Sample Return Missions: How, Where, and What Do We Do with the Rocks? Aurore Hutzler Horizon 2061 – 11-13 September 2019 - Toulouse Exploring Space through Sample Return Missions: The Vital Role of Curation Aurore Hutzler Horizon 2061 – 11-13 September 2019 - Toulouse Geologist by training in analytical geochemistry Ph.D. in France on meteorite terrestrial ages Post-doc in Austria on the ideal curation facility for astromaterials Now Visiting Scientist at the Curation Office, NASA JSC (Houston, Texas) on contamination control and knowledge and material suitability. Outline • Where have we been so far? • Exploration of the Solar System: why do we need sample return missions? • NASA Astromaterials Acquisition and Curation Office • Upcoming sample return missions and needed facilities • Where do we want to go next • How curation should adapt to new challenges Looking above Early observations of moons and planets Remote and in-situ missions (1950’s) Where have we been so far? Itokawa Hayabusa (2010) Comet 81P/Wild Stardust (2006) Moon Earth-Sun Lagrange 1 Apollo 11 to 17 (1969-1972) Genesis (2004) Luna 16, 20, 24 (1970-1976) Falling from above Meteorites are from space (1794) Where have we been so far (sort of)? Moon Mars (SNC meteorites) Vesta (HED meteorites) Why sample return missions? • Meteorite studies have limitations: • Rock types and ages • Geological context • Alteration via ejection and trip back to Earth • Fabulous new discoveries from in-situ and remote studies have raised questions that require complementary analyses. • Preparation techniques in terrestrial laboratories allow for analyses at higher spatial resolution and precision. • Analytical instrumentation and techniques on Earth are more flexible and constantly innovating.
    [Show full text]
  • PDS Roadmap, 2006-2016
    Planetary Data System Strategic Roadmap 2006 - 2016 PDS Management Council Planetary Data System Mission To facilitate achievement of NASA’s planetary science goals by efficiently archiving and making accessible digital data produced by or relevant to NASA’s planetary missions, research programs, and data analysis programs. Feb 2006 http://pds.nasa.gov/ Topics Covered in This Presentation NASA’s Vision for the Planetary Data System (PDS) Characteristics of The PDS Missions in Progress Current Challenges Ongoing Challenges Requirements Functions Implementation PDS Realities The PDS 5-year Goals Milestones to Implement PDS in 5 Years Feb 2006 PDS Strategic Roadmap - 2 NASA’s Vision for the PDS To gather and preserve the data obtained from exploration of the Solar System by the U.S. and other nations To facilitate new and exciting discoveries by providing access to and ensuring usability of those data to the worldwide community To inspire the public through availability and distribution of the body of knowledge reflected in the PDS data collection To support the NASA vision for human and robotic exploration of the Solar System by providing an online scientific data archive of the data resources captured from NASA’s missions Feb 2006 PDS Strategic Roadmap - 3 Characteristics of the PDS Data Archive The PDS archives and makes available space-borne, ground-based, and laboratory experiment data from over 50 years of NASA-based exploration of comets, asteroids, moons, and planets. The archives include data products derived from a very wide range of measurements, e.g., imaging experiments, gravity and magnetic field and plasma measurements, altimetry data, and various spectroscopic observations.
    [Show full text]
  • Busiest Year Coming Up, Elachi Says Director Delivers ‘State of the Lab’ Address
    Jet NOVEMBER Propulsion 2008 Laboratory VOLUME 38 NUMBER 11 Busiest year coming up, Elachi says Director delivers ‘State of the Lab’ address By Mark Whalen Carol Carol Lachata / JPL Photo Lab With 19 spacecraft currently in operation across did “an excellent job” negotiating a major contract for Atmosphere and Volatile Evolution mission, a Goddard the solar system, JPL won’t be resting on its laurels the project. “It’s not only the technical people on MSL Space Flight Center–managed, principal investigator anytime soon. In his semiannual state of the Labo- who are critical, it’s everybody,” Elachi said. mission set for a 2013 launch. NASA is also planning a ratory address Oct. 27, JPL Director Charles Elachi The director noted that because more funds were Mars 2016 mission, most likely with a lander and rover. told employees to expect the busiest year ever in needed for Mars Science Laboratory to make its launch, “This will probably need to be defined within the next fiscal 2009. some projects were asked to minimize their budget car- six months,” he said. Noting that this next set of challenges is un- ryover into next year. This action, he said, will not im- JPL’s astrophysics efforts will move forward with derway with the Oct. 22 launch of India’s Chan- pact any project or its funding need for this year. NuStar, Wide-field Infrared Survey Explorer and Kepler drayaan-1, which includes JPL’s Moon Mineralogy Overall, JPL is in “reasonably good shape,” Elachi fully funded. Elachi also noted that NASA has decided Mapper instrument, Elachi said JPL will launch said, despite uncertainty with respect to the NASA bud- JPL will manage an upcoming exoplanet mission, with four missions in calendar year 2009 along with sig- get.
    [Show full text]
  • INVESTIGATING YOUNG (<100 MILLION YEARS) IRREGULAR
    47th Lunar and Planetary Science Conference (2016) 2106.pdf INVESTIGATING YOUNG (<100 MILLION YEARS) IRREGULAR MARE PATCHES ON THE MOON USING MOON MINERALOGY MAPPER OBSERVATIONS. J. Grice1, K. L. Donaldson Hanna1, N. E. Bowles1, P. H. Schultz2, and K. A. Bennett3, 1Atmospheric, Oceanic and Planetary Physics, University of Oxford, Clarendon Laboratory, Oxford, UK ([email protected]), 2Dept. of Earth, Environmental and Plane- tary Sciences, Brown University, Providence, RI, USA, and 3School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA. Introduction: The investigation and characteriza- these features and the evolution of lunar basalts over tion of volcanism on a planetary surface provides the time. Compositional differences across each IMP as best insight into the composition, structure, and thermal well as differences with surrounding mare materials history of its interior. The lunar maria, vast plains are investigated using visible to near infrared (VNIR) formed of basaltic flows, are limited to and cover 17% observations from the Moon Mineralogy Mapper (M3) of the lunar near side [1]. Radiometric age dating of instrument. returned Apollo samples and crater counts from remote Data and Methods: M3, an imaging spectrometer observations indicates that mare basaltic volcanism was onboard the Chandrayaan-1 spacecraft, mapped the active from ~4.2 to 0.8 Ga [e.g. 2-5]. lunar surface across the VNIR (0.43-3.0μm) in 85 Lunar-Orbiter/Apollo images and Clementine bands [9]. The focus of this initial analysis is on the UVVIS observations identified four regions, including two largest IMPs, Sosigenes (max length of 5 km) and Ina, of small-scale, low relief patches of rubble with a Ina (diameter of 3 km).
    [Show full text]
  • Complete Dissertation
    VU Research Portal The lunar crust Martinot, Melissa 2019 document version Publisher's PDF, also known as Version of record Link to publication in VU Research Portal citation for published version (APA) Martinot, M. (2019). The lunar crust: A study of the lunar crust composition and organisation with spectroscopic data from the Moon Mineralogy Mapper. General rights Copyright and moral rights for the publications made accessible in the public portal are retained by the authors and/or other copyright owners and it is a condition of accessing publications that users recognise and abide by the legal requirements associated with these rights. • Users may download and print one copy of any publication from the public portal for the purpose of private study or research. • You may not further distribute the material or use it for any profit-making activity or commercial gain • You may freely distribute the URL identifying the publication in the public portal ? Take down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. E-mail address: [email protected] Download date: 10. Oct. 2021 VRIJE UNIVERSITEIT THE LUNAR CRUST A study of the lunar crust composition and organisation with spectroscopic data from the Moon Mineralogy Mapper ACADEMISCH PROEFSCHRIFT ter verkrijging van de graad Doctor of Philosophy aan de Vrije Universiteit Amsterdam, op gezag van de rector magnificus prof.dr. V. Subramaniam, in het openbaar te verdedigen ten overstaan van de promotiecommissie van de Faculteit der Bètawetenschappen op maandag 7 oktober 2019 om 13.45 uur in de aula van de universiteit, De Boelelaan 1105 door Mélissa Martinot geboren te Die, Frankrijk promotoren: prof.dr.
    [Show full text]
  • Intergrating Morpho-Stratigraphic and Spectral Units on Mercury and the Moon: Updates from the PLANMAP Project
    EGU2020-19741 https://doi.org/10.5194/egusphere-egu2020-19741 EGU General Assembly 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. Intergrating morpho-stratigraphic and spectral units on Mercury and the Moon: Updates from the PLANMAP project Cristian Carli1, Francesca Zambon1, Francesca Altieri1, Carlos Brandt2, Angelo Pio Rossi2, and Matteo Massironi3 1INAF - IAPS, Via del Fosso del Cavaliere, 100, I-00133 Rome, Italy ([email protected]) 2Jacobs University, gGmbH Campus Ring 1 28759, Bremen, Germany 3University of Padua, Department of Geoscience, Via Gradenigo 6, I-35131 Padua, Italy The numerous past and present space missions dedicated to the Solar System planetary bodies exploration, provided a huge amount of data so far. In particular, data acquired by cameras and spectrometers allowed for producing morpho-stratigraphic and mineralogical maps for many planets, satellites and minor bodies. Despite the considerable progresses, the integration of these products is still poorly addressed. To date, no geological maps of planetary bodies other than the Earth, containing both the information, are available yet. In this context, one of the main goals the “European Union's Horizon 2020 - PLANetary MAPping (PLANMAP)” project [1] is to provide, for the first time, highly informative geological maps of specific regions of interest on the Moon, Mercury and Mars, taking into account datasets publicly available in the Planetary Data System (PDS) database [2]. Here, we show the results achieved during the first two years of the project by the PLANMAP “Compositional unit definition Work Package”. In particular, we focused on specific areas, such as Hokusai quadrangle (22°-60° N, 0°-90°W) and Beethoven (13.24°S- 28.39° S; 116.1°- 132.32°W, 630 km diameter) and Rembrandt (24.58°S- 41.19°S, 261.72°- 282.73°W, 716 km diameter) basins on Mercury, and the Apollo basin (10 ° –60 ° S, 125 ° –175 ° W, 492 km diameter) within the northeastern edge of the ~ 2500 km South Pole-Aitken (SPA) basin on the Moon [3].
    [Show full text]
  • Global Distribution and Characteristics of Domical
    50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1803.pdf GLOBAL DISTRIBUTION AND CHARACTERISTICS OF DOMICAL CRATERS ON THE MOON Nandita Kumari1,2, Harish Nandal2, Indhu Varatharajan3, Ritu Anilkumar4, Kanmani Shanmugapriya1 and Vijayan S2 1Institute of Remote Sensing, Anna University, Chennai (Email: [email protected]), 2Physical Research Laboratory, PSDN, Ahmedabad, 3Institute of Planetary Research, DLR, Berlin, 4North-Eastern Space Application Centre, Meghalaya Introduction: On Moon, there are reports of small to GRAIL crustal thickness map in our study. Using large scale domes which are the result of extrusive Jowiak [3] as an initial reference, the identified FFCs volcanism [1,2]. Such domes are present within mare were examined to distinguish those with convex-up regions and predominantly associated to same [1]. uplift spread across the entire floor (Fig. 1). However, dome like structures or convex up floors have Consequently, we undertook a global survey of the also been reported inside some craters with fractures on LROC Wide-Angle Camera (WAC) data overlaid on it, under the class of Floor Fracture Craters(FFCs)[3,4]. LOLA-SELENE Merger data to identify those domical Domical craters are a class of lunar craters defined by craters and identified 16 such craters (Fig. 2). their distinctly convex-up uplifted, often reverted bowl like floors. The dome inside these craters make them an ideal candidate to study the evolution and influence of underlying stalled magma in a constrained condition which are likely present over different parts of moon. Moreover, craters with domical floor uplift will provide significant information about the intrusions that occurred into the lunar crust [3,4].
    [Show full text]
  • Commerce, Justice, Science, and Related Agencies Appropriations for Fiscal Year 2010
    S. HRG. 111–187 COMMERCE, JUSTICE, SCIENCE, AND RELATED AGENCIES APPROPRIATIONS FOR FISCAL YEAR 2010 HEARINGS BEFORE A SUBCOMMITTEE OF THE COMMITTEE ON APPROPRIATIONS UNITED STATES SENATE ONE HUNDRED ELEVENTH CONGRESS FIRST SESSION ON H.R. 2847 AN ACT MAKING APPROPRIATIONS FOR THE DEPARTMENTS OF COM- MERCE AND JUSTICE, SCIENCE, AND RELATED AGENCIES FOR THE FISCAL YEAR ENDING SEPTEMBER 30, 2010, AND FOR OTHER PUR- POSES Department of Commerce Department of Justice National Aeronautics and Space Administration Nondepartmental Witnesses Printed for the use of the Committee on Appropriations Available via the World Wide Web: http://www.gpoaccess.gov/congress/index.html U.S. GOVERNMENT PRINTING OFFICE 48–287 PDF WASHINGTON : 2009 For sale by the Superintendent of Documents, U.S. Government Printing Office Internet: bookstore.gpo.gov Phone: toll free (866) 512–1800; DC area (202) 512–1800 Fax: (202) 512–2104 Mail: Stop IDCC, Washington, DC 20402–0001 COMMITTEE ON APPROPRIATIONS DANIEL K. INOUYE, Hawaii, Chairman ROBERT C. BYRD, West Virginia THAD COCHRAN, Mississippi PATRICK J. LEAHY, Vermont CHRISTOPHER S. BOND, Missouri TOM HARKIN, Iowa MITCH MCCONNELL, Kentucky BARBARA A. MIKULSKI, Maryland RICHARD C. SHELBY, Alabama HERB KOHL, Wisconsin JUDD GREGG, New Hampshire PATTY MURRAY, Washington ROBERT F. BENNETT, Utah BYRON L. DORGAN, North Dakota KAY BAILEY HUTCHISON, Texas DIANNE FEINSTEIN, California SAM BROWNBACK, Kansas RICHARD J. DURBIN, Illinois LAMAR ALEXANDER, Tennessee TIM JOHNSON, South Dakota SUSAN COLLINS, Maine MARY L. LANDRIEU, Louisiana GEORGE V. VOINOVICH, Ohio JACK REED, Rhode Island LISA MURKOWSKI, Alaska FRANK R. LAUTENBERG, New Jersey BEN NELSON, Nebraska MARK PRYOR, Arkansas JON TESTER, Montana ARLEN SPECTER, Pennsylvania CHARLES J.
    [Show full text]
  • Moon Mineralogy Mapper
    JPL D-39032 Moon Mineralogy Mapper DATA PRODUCT SOFTWARE INTERFACE SPECIFICATION Version 9.10 November 22, 2011 Prepared by: Sarah Lundeen JPL Stephanie McLaughlin UMD Rafael Alanis PDS Imaging Node 1 Approved by: ________________________ Carle Pieters, M3 Principal Investigator ________________________ Sue Lavoie, Director PDS Imaging Node _______________________ Edwin Grayzeck, PDS Project Manager ________________________ Sarah Lundeen, M3 Instrument Ground Data System ________________________ Jessica Sunshine, M3 Level 2 Archive Lead 2 TABLE OF CONTENTS 1. Introduction ....................................................................................................................................... 11 1.1. Purpose and Scope .................................................................................................................... 11 1.2. Contents ..................................................................................................................................... 11 1.3. Applicable Documents and Constraints ................................................................................... 11 1.4. Relationships with Other Interfaces ......................................................................................... 13 1.5. Image Display and Analysis Software – ENVI/IDL ............................................................... 13 2. DATA PRODUCT CHARACTERISTICS AND ENVIRONMENT ............................................ 14 2.1. Instrument Overview ...............................................................................................................
    [Show full text]
  • Senate Hearings Before the Committee on Appropriations
    S. HRG. 111–999 Senate Hearings Before the Committee on Appropriations Commerce, Justice, Science, and Related Agencies Appropriations Fiscal Year 2011 111th CONGRESS, SECOND SESSION S. 3636 DEPARTMENT OF COMMERCE DEPARTMENT OF JUSTICE NATIONAL AERONAUTICS AND SPACE ADMINISTRATION NONDEPARTMENTAL WITNESSES Commerce, Justice, Science, and Related Agencies, 2011 (S. 3636) S. HRG. 111–999 COMMERCE, JUSTICE, SCIENCE, AND RELATED AGENCIES APPROPRIATIONS FOR FISCAL YEAR 2011 HEARINGS BEFORE A SUBCOMMITTEE OF THE COMMITTEE ON APPROPRIATIONS UNITED STATES SENATE ONE HUNDRED ELEVENTH CONGRESS SECOND SESSION ON S. 3636 AN ACT MAKING APPROPRIATIONS FOR THE DEPARTMENTS OF COM- MERCE AND JUSTICE, AND SCIENCE, AND RELATED AGENCIES FOR THE FISCAL YEAR ENDING SEPTEMBER 30, 2011, AND FOR OTHER PURPOSES Department of Commerce Department of Justice National Aeronautics and Space Administration Nondepartmental Witnesses Printed for the use of the Committee on Appropriations ( Available via the World Wide Web: http://www.gpo.gov/fdsys U.S. GOVERNMENT PRINTING OFFICE 54–959 PDF WASHINGTON : 2011 For sale by the Superintendent of Documents, U.S. Government Printing Office Internet: bookstore.gpo.gov Phone: toll free (866) 512–1800; DC area (202) 512–1800 Fax: (202) 512–2104 Mail: Stop IDCC, Washington, DC 20402–0001 COMMITTEE ON APPROPRIATIONS DANIEL K. INOUYE, Hawaii, Chairman ROBERT C. BYRD, West Virginia THAD COCHRAN, Mississippi PATRICK J. LEAHY, Vermont CHRISTOPHER S. BOND, Missouri TOM HARKIN, Iowa MITCH MCCONNELL, Kentucky BARBARA A. MIKULSKI, Maryland RICHARD C. SHELBY, Alabama HERB KOHL, Wisconsin JUDD GREGG, New Hampshire PATTY MURRAY, Washington ROBERT F. BENNETT, Utah BYRON L. DORGAN, North Dakota KAY BAILEY HUTCHISON, Texas DIANNE FEINSTEIN, California SAM BROWNBACK, Kansas RICHARD J.
    [Show full text]