The Collier Report of U.S. Government Contracting

Sampling of Federal Government Funding Actions/Set Asides

In order by amount of set aside monies.

• $99,000 - Thursday the 13th of December 2012
  National Institutes Of Health
  NIH, NIDA, OD OM OA OFC ACQUISITIONS
  IGF::OT::IGF PROTEOMIC ASSAYS

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• $98,027 - Tuesday the 31st of July 2012
  Veterans Affairs Department
  573-NF/SG VETERANS HEALTH SYSTEM
  PROFESSIONAL SERVICES TO ASSIST IN THE INTERVENTION TARGETED TO VETERANS WITH DIMINTIA.

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• $97,859 - Thursday the 28th of May 2015
  National Aeronautics And Space Administration
  NASA SHARED SERVICES CENTER
  DEBRIS DISKS ARE OPTICALLY THIN, ALMOST GAS-FREE DUSTY DISKS OBSERVED AROUND A SIGNIFICANT FRACTION OF MAIN-SEQUENCE STARS OLDER THAN ABOUT 10 MYR. SINCE THE CIRCUMSTELLAR DUST IS SHORT-LIVED, THE VERY EXISTENCE OF THESE DISKS IS CONSIDERED AS EVIDENCE THAT DUST-PRODUCING PLANETESIMALS ARE STILL PRESENT IN SYSTEMS IN WHICH ARE FORMING - OR HAVE FAILED TO FORM - A LONG TIME AGO. OUR WORK ON THIS PROPOSAL WILL PERFORM A UNIFIED SEARCH OF THE SPITZER AND ISO DATA ARCHIVES FOR GOOD DEBRIS DISK SPECTRAL CANDIDATES, ATTEMPTING TO PLACE THEM INTO THE GENERAL CONTEXT OF PLANETARY SYSTEMS, UNCOVERING INTERRELATIONS BETWEEN THE DISKS, DUST PARENT BODIES, AND PLANETS. WE PROPOSE MINING THE SPITZER AND ISO DATA ARCHIVES TO SEARCH FOR HIGH SNR, HIGH SPECTRAL FEATURE CONTRAST IRS 5-35 UM SPECTRA OF DUST DISKS AROUND (MAINLY) YOUNG STARS IN THE THROWS OF BUILDING AND EVOLVING PLANETS. ARCHIVAL DATA SPECTRA WILL BE ANALYZED FOR THE AMOUNT, SIZE, LOCATION,&COMPOSITION OF THE DUST&ANY REMNANT GAS. THE REMOTE SENSING ANALYSIS IS BASED ON THE RESULTS OF THE DEEP IMPACT EXCAVATION EXPERIMENT&THE STARDUST SAMPLE RETURN EXPERIMENTS,&IS THUS BOTH NOVEL&EXPERIMENTALLY VERIFIABLE. ADDITIONAL INFORMATION ON THE BEHAVIOR AND EFFECTS OF THE PRIMARY ON THE DISK WILL BE GLEANED FROM THE IRAS, COBE, MSX, 2MASS, SDSS, PANSTARRS, AND ROSAT, CHANDRA, AND XMM ARCHIVES. WE WILL ESPECIALLY TARGET NEARBY YOUNG, BRIGHT STARS WITH UNUSUALLY HIGH AMOUNTS OF WARM CIRCUMSTELLAR DUST&GAS FORMED BY HIGH TEMPERATURE PROCESSES LIKE STELLAR FLARES, NEBULAR SHOCKS, COLLISIONAL GRINDING,&GIANT IMPACTS. WE WILL EXPLORE THE IMPLICATIONS OF THE DERIVED COMPOSITION FOR THE FORMATION OF THE DUST IN THE PROTO-PLANETARY DISK AND THE SUBSEQUENT EFFECTS OF AGGREGATION, THERMALIZATION,&PLANETISIMAL FORMATION. OUR STUDIES TO DATE HAVE DETECTED EVIDENCE OF TERRESTRIAL PLANET BUILDING, CATASTROPHIC DISRUPTION OF AN ASTEROID YIELDING A DENSE ZODY CLOUD,&A GIANT HYPERVELOCITY IMPACT EVENT IN NEARBY YOUNG STAR SYSTEMS, SHOWING THAT DEBRIS DISKS CAN SERVE AS TRACERS OF PLANETESIMALS AND PLANETS, PROVIDING CLUES TO THE PLANETESIMAL AND PLANET FORMATION PROCESSES THAT OPERATED IN THESE SYSTEMS IN THE PAST.

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• $97,381 - Monday the 29th of June 2015
  National Aeronautics And Space Administration
  NASA SHARED SERVICES CENTER
  HIGH-RESOLUTION SPECTRAL MAPPING OF VALLES MARINERIS SUMMARY: VALLES MARINERIS CONTAINS EXPOSURES OF GEOLOGIC UNITS CRITICAL TO UNDERSTANDING THE COMPOSITION AND STRUCTURE OF MARS' CRUST, AND THE ROLE OF AQUEOUS ENVIRONMENTS IN MODIFYING THE SURFACE AND SUBSURFACE. THE WALLS OF THE CHASMA SYSTEM EXPOSE THE ENTIRE SECTION OF THE NOACHIAN-HESPERIAN AGED PLATEAU PLAINS (ENCOMPASSING UNITS HNU THROUGH HPL3), INCLUDING EXAMPLES OF MAJOR LITHOLOGIES SEEN ELSEWHERE ON MARS THAT FORM THE FRAMEWORK OF THE CRUST. THESE INCLUDE BASALTS, LOW-CA PYROXENE AND OLIVINE-BEARING ULTRAMAFIC ROCKS, AND PHYLLOSILICATES FORMED DURING AN EARLY PERIOD OF AQUEOUS ALTERATION. COMPARED TO EXPOSURES OF CRUSTAL LAYERING IN HIGHLAND CRATERS AND BASINS, THE SECTION IN THE CHASMA WALLS IS RELATIVELY INTACT. THE INTERIOR LAYERED DEPOSITS CONTAIN ONE OF MARS' TWO KNOWN REGIONAL OCCURENCES SULFATE MINERALS OF VARIOUS COMPOSITION, FORMED DURING A LATER PERIOD OF AQUEOUS ACTIVITY. FINALLY. THE SURROUNDING PLATEAU CONTAINS THIN SUPERPOSED, LIGHT-TONED LAYERED DEPOSITS RECENTLY SHOWN FROM CRISM DATA TO CONTAIN A THIRD MAJOR AQUEOUS MINERALOGY, HYDRATED SILICA. IN ORDER TO BETTER UNDERSTAND THE FORMATION OF MARS' CRUST AND THE RECORD OF THE PLANET'S AQUEOUS PROCESSES AS EXPOSED AT VALLES MARINCRIS, WE PROPOSE TO: - CREATE AND DELIVER TO THE PDS AS SERIES OF HIGH-RESOLUTION MOSAICS OF CRISM MULTISPECTRAL AND TARGETED OBSERVATIONS, COVERING PARTS OF THE CHASMA SYSTEM WITH A HIGH DENSITY OF TARGETED OBSERVATIONS, AND USING THESE MAPS, - INVESTIGATE THE VERTICAL STRATIGRAPHY OF THE PLATEAU PLAINS SERIES EXPOSED INTACT IN THE CHASMA WALLS, - DETERMINE THE VERTICAL AND LATERAL DISTRIBUTION OF PHYLLOSILICATES EXPOSED IN THE WALLS, AND HOW THEY COMPARE TO OTHER EXPOSURES IN NOACHIAN TERRAIN, AND - COMPARE THE VERTICAL STRATIGRAPHY AND COMPOSITIONAL LAYERING OF THE ERODED PLATEAU OF INTERIOR LAYERED DEPOSITS IN TITHONIUM CHASMA WITH COMPARABLE DEPOSITS IN CANDOR AND JUVENTAE CHASMATA.

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• $968,118 - Tuesday the 21st of April 2015
  National Institutes Of Health
  NIH, NHLBI, DERA OA OFC ACQUISTIONS
  IGF::OT::IGF OTHER FUNCTIONS: GWAS HUMANOMNIEXPRESS PLUS EXOME WITH PLATE ALIQUOTING FOR NIEHS (WEINBURG)

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• $96,246 - Thursday the 5th of November 2015
  National Aeronautics And Space Administration
  NASA SHARED SERVICES CENTER
  THE PLANETARY SATELLITES EUROPA AND GANYMEDE ARE CONTINUOUSLY OVERTAKEN IN THEIR ORBITS BY THE COROTATING PLASMA TRAPPED BY THE MAGNETIC FIELD OF JUPITER. THIS INTERACTION BETWEEN THE MAGNETOSPHERE AND EUROPA'S SURFACE LEADS TO THE FORMATION OF A CIRCUMPLANETARY TORUS OF NEUTRALS. THE NEUTRAL TORUS HAS BEEN OBSERVED REMOTELY AND ALSO THROUGH THE ANALYSIS OF DATA OBTAINED BY THE GALILEO SPACECRAFT WHILE IN ORBIT. ONE HYPOTHESIS ON THE FORMATION OF THIS TORUS IS THAT DIRECT WEATHERING OF THE SURFACE OF EUROPA IS TAKING PLACE AT A HIGH RATE. PROCESSES SUCH AS SPUTTERING BY ENERGETIC HEAVY IONS APPARENTLY POPULATE THE LOCAL ENVIRONMENT OF THIS MOON. THESE SPUTTER PRODUCTS CAN BE CARRIED FURTHER AROUND THE PLANET BY THE ACTION OF PLASMA FLOW ONTO AND AROUND EUROPA. HOWEVER, THERE ARE REASONS TO DOUBT THIS PICTURE. FOR INSTANCE, AT LEAST ONE RECENT SIMULATION SUGGESTS THAT PLASMA FLOW UPSTREAM AND OVER EUROPA IS VERY SLOW, LIMITING THE RATE AT WHICH NEW WEATHERING AGENTS CAN BE BROUGHT INTO CONTACT WITH THE SURFACE AND LIMITING THE RATE AT WHICH NEUTRALS CAN BE DRIVEN INTO CIRCUMPLANETARY ORBITS. THESE NEUTRALS HAVE LIMITED LIFETIMES PARTLY BECAUSE OF INTERACTIONS WITH HOT PLASMA ELECTRONS. THE WEATHERING OF GANYMEDE'S SURFACE IS COMPLETELY DIFFERENT. THERE AN INTERNALLY-GENERATED MAGNETIC FIELD PARTIALLY SHIELDS THE SURFACE FROM DIRECT WEATHERING BY THE JOVIAN MAGNETOSPHERE. INSTEAD ONLY THE GANYMEDE POLAR REGIONS ARE MAGNETICALLY CONNECTED TO JUPITER'S FIELD, GIVING MAGNETOSPHERIC FLUX SOME DIRECT ACCESS TO THE SURFACE. THE EQUATORIAL SURFACE OF GANYMEDE IS THREADED BY CLOSED GANYMEDE FIELD LINES AND ONLY A FRACTION OF THE CHARGED PARTICLES IN THE SURROUNDING MEDIUM CAN GAIN ACCESS TO THIS PART OF THE SURFACE. RECENT STUDIES HAVE CORRELATED THE OPEN MAGNETIC FIELD REGION NEAR THE GANYMEDE POLES TO BRIGHTER SURFACE FEATURES DETECTED WITH OPTICAL REMOTE SENSING. THE RELATIONSHIP BETWEEN THE BRIGHT POLAR CAPS AND OPEN FIELD LINES SUGGESTS THAT CHARGED WEATHERING AGENTS ARE RESPONSIBLE FOR THE BRIGHTENING. IT IS LESS CLEAR WHICH PARTICLES (ELECTRONS OR IONS) BRIGHTEN THE ICE OR WHAT THE MOST CRITICAL PARTICLE ENERGIES ARE. IN THIS PROPOSAL, WE WILL USE DATA OBTAINED BY THE GALILEO SPACECRAFT'S ENERGETIC PARTICLES DETECTOR (EPD) TO ADDRESS THESE QUESTIONS. FOR EUROPA, OUR GOAL IS TO UNDERSTAND THE FLOW ONTO AND OVER THE MOON TO DETERMINE WHETHER THE PICTURE OF SURFACE WEATHERING THAT HAS BEEN PUT FORWARD CAN ACCOUNT FOR THE EXTENDED NEUTRAL GAS TORUS. FOR GANYMEDE, WE WILL ANALYZE THE EPD DATA SET TO CORRELATE WEATHERING AGENTS WITH SURFACE PROPERTIES. WE ARE LOOKING, FOR INSTANCE, AT WHICH SPECIES AND ENERGIES CORRESPOND TO PRECIPITATING FLUX THAT IS BOTH FAIRLY CONSTANT OVER THE POLAR CAPS BUT COMPLETELY DIFFERENT ON CLOSED FIELD LINES. GALILEO HAD MANY CLOSE FLYBYS OF EUROPA AND GANYMEDE AND TOOK HIGH TIME RESOLUTION DATA IN THE NEAR-SURFACE ENVIRONMENT OF BOTH MOONS. THIS PROPOSAL IS CONSISTENT WITH THE GOALS OF NASA'S OUTER PLANETS RESEARCH PROGRAM INCLUDING EXPANDING THE RETURN OF GALILEO MISSION DATA AND EXPLORING PROCESSES RELATING TO THE PLANETARY SATELLITES AND THE EVOLUTION OF THEIR VISIBLE SURFACES. EUROPA AND GANYMEDE ARE ALSO TWO POTENTIAL TARGETS FOR FUTURE ORBITING SPACECRAFT AND THIS PROPOSAL WILL INCREASE OUR UNDERSTANDING OF THE NEAR-SURFACE ENVIRONMENT OF EACH OF THEM.

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• $96 - Wednesday the 27th of June 2012
  Department Of Navy
  NAVY MEDICINE PROFESSIONAL
  TUITION AND FEES

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• $9,597 - Monday the 17th of September 2012
  Department Of Army
  W4PZ USA MED RSCH ACQUIS ACT
  ALTERNATIVE ARTHROPOD REPELLENT MATERIAL

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• $95,000 - Saturday the 1st of December 2012
  National Institutes Of Health
  NIH, NHLBI, DERA OA OFC ACQUISTIONS
  IGF::CT::IGF 2:CRITICAL FUNCTION/CLINICAL TRAINING FOR THE NEXT GENOME FELLOWS

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• $94,000 - Friday the 10th of July 2015
  National Aeronautics And Space Administration
  NASA SHARED SERVICES CENTER
  AN ACCURATE UNDERSTANDING OF COMPOSITION AND ITS VARIATION IS A FUNDAMENTAL TOOL NECESSARY FOR GEOLOGIC INTERPRETATION OF ANY PLANETARY BODY. THEORETICAL TECHNIQUES OF HAPKE [1981; 1993; 2001] ALLOW A QUANTITATIVE ANALYSIS OF ULTRAVIOLET, VISIBLE, AND NEAR-INFRARED SPECTRAL REFLECTANCE DATA SETS (LABORATORY AND SPACECRAFT). THESE METHODS DEMAND A PRECISE UNDERSTANDING OF THE INTERACTION OF ELECTROMAGNETIC RADIATION (I.E., LIGHT) WITH MINERALS OF VARYING CHEMISTRIES [LUCEY, 1998; DENEVI ET AL., 2007]. THIS UNDERSTANDING IS CAPTURED IN THE OPTICAL CONSTANTS (N AND K) OF MINERALS, WHICH ARE FUNDAMENTAL TO MODELING SPECTRAL PROPERTIES OF PLANETARY SURFACES [HAPKE, 1993]. SEVERAL STUDIES DETAIL THE PROMISE AND SHORTCOMINGS OF THESE SPECTRAL ANALYSIS TECHNIQUES, TESTING THEM BY MODELING SPECTRA OF THOROUGHLY CHARACTERIZED LUNAR SOIL AND METEORITE SAMPLE SUITES [LAWRENCE AND LUCEY, 2007; DENEVI ET AL., 2008; CAHILL ET AL., 2010]. THESE SHORTCOMINGS INCLUDE THE USE OF A SMALL DATABASE OF MINERAL OPTICAL CONSTANTS ALLOWING FOR ONLY LIMITED EMPIRICAL KNOWLEDGE OF MINERAL OPTICAL CONSTANT VARIATION WITH CHANGING CHEMISTRY (IN PARTICULAR CALCIUM, IRON, AND MAGNESIUM) AND A GENERAL LACK OF KNOWLEDGE WITHIN THE ULTRAVIOLET PORTION OF THE SPECTRUM [LUCEY, 1998; DENEVI ET AL., 2007]. CONSIDERING THE DIVERSITY OF PYROXENE AND OLIVINE CHEMISTRIES AND RESULTING DIFFERENCES IN THEIR REPRESENTATIVE SPECTRA THESE SHORTCOMINGS SEVERELY LIMIT THE EFFECTIVENESS OF CURRENT MODELING TECHNIQUES. HERE WE WILL DETERMINE OPTICAL CONSTANTS FROM LABORATORY-MEASURED SPECTRA OF MINERALS RELEVANT FOR EFFECTIVE ANALYSIS OF ROCKY BODIES (I.E., MOON, MERCURY, MARS, VESTA, ETC.). OPTICAL CONSTANTS WILL BE DETERMINED FOR THE CRITICALLY IMPORTANT MINERALS PYROXENE AND OLIVINE. A SUITE OF SYNTHETICALLY DERIVED AND RIGOROUSLY CHARACTERIZED PYROXENE AND OLIVINE SAMPLES WILL BE USED FOR THESE STUDIES [TURNOCK ET AL., 1973; KLIMA ET AL., 2007; 2008; DYAR ET AL., 2009]. THESE DATA WILL THEN BE INTEGRATED INTO EXISTING MODELS AND TESTED ON WELL- CHARACTERIZED SYNTHETIC, LUNAR SOIL, AND METEORITE PLANETARY DATA SETS FOR ACCURACY. THESE STEPS WILL PROVE CRITICAL FOR SUPPORTING DATA ANALYSIS EFFORTS OF ONGOING PLANETARY MISSION MULTI- AND HYPERSPECTRAL REFLECTANCE PAYLOADS CARRIED BY THE LUNAR RECONNAISSANCE ORBITER (WIDE ANGLE CAMERA), KAGUYA/SELENE (MULTI-SPECTRAL IMAGER AND SPECTRAL PROFILER), CHANG E-1, CHANDRAYAAN-1 (MOON MINERALOGIC MAPPER), MESSENGER (MERCURY ATMOSPHERIC AND SURFACE COMPOSITION SPECTROMETER AND MERCURY DUAL IMAGING SYSTEM), MARS RECONNAISSANCE ORBITER (COMPACT RECONNAISSANCE IMAGING SPECTROMETER FOR MARS), NEAR, AND DAWN (VISIBLE AND INFRARED SPECTROMETER).

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