University of Tennessee
Who it subcontracts to
No subawards reported under its lunar awards.
Who it works for
THE PURPOSE OF THIS SUBCONTRACT AWARD IS FOR THE UNIVERSITY OF TENNESSEE, KNOXVILLE (UTK) TO SUPPORT THE UNIVERSITY OF NEW HAMPSHIRE (UNH) PHASE E EFFORT ON THE COSMIC RAY TELESCOPE FOR THE EFFECT OF RADIATION (CRATER) INSTRUMENT FOR THE LUNAR RECONNAISSANCE ORBITER (LRO) MISSION. UTK SHALL CONTINUE TO DEVELOP STATE-OF-THE-ART NUMERICAL MODELS OF RADIATION INTERACTION WITH MATTER, COMPARE THESE MODELS WITH CRATER OBSERVATIONS, SUPPORT PRESENTATION OF THESE RESULTS AT CRATER AND LRO TEAM MEETINGS, AND PREPARE THEM FOR PUBLICATION IN THE REFEREED LITERATURE.
- Auburn University$350K
COLD-TOLERANT ELECTRONICS AND PACKAGING FOR LUNAR SURFACE EXPLORATION
DR. LAWRENCE TAYLOR WILL SUPPORT THE EDUCATION PUBLIC I ENGAGEMENT (EPE) EFFORT OF THE UNIVERSITY OF CENTRAL FLORIDA CENTER FOR LUNAR AND ASTEROID SURFACE SCIENCE (CLASS) SOLAR SYSTEM EXPLORATION RESEARCH VIRTUAL INSTITUTE (SSERVI) UNDER THE DIRECTION OF PI, DR. DANIEL BRITT. AS PART OF THIS EFFORT, DR. LAWRENCE TAYLOR WILL" 1) ATTEND UCF/CLASS- SSERVI SCIENCE TEAM MEETINGS AT THE UNIVERSITY OF CENTRAL FLORIDA AND ELSEWHERE AS CALLED UPON BY THE PI, DR. DANIEL BRITT 2) WORK CLOSELY WITH UCF/CLASS SCIENCE TEAM MEMBERS AND PARTNERS TO CREATE, REVIEW, TEST, MODIFY AND DISTRIBUTE EPE CURRICULA AND ACTIVITIES ACCORDING TO THE TIMELINE IN THE PROPOSAL: SOME TRAVEL MAY BE INVOLVED. 3) FACILITATE COMMUNICATION BETWEEN THE SSERVI CENTRAL EPE OFFICE, THE OTHER SSERVI EPE TEAMS AND THE CLASS TEAM AS APPROPRIATE. 4) REPRESENT THE UCF/CLASS SSERVI EPE TEAM AT SSERVI MEETINGS, EPE EVENTS AND EDUCATOR WORKSHOPS, AND ELSEWHERE AS CALLED UPON BY THE PI 5) BE PRESENT AND ASSIST THE UCF/CLASS TEAM WITH EPE PRESENTATIONS AT MEETINGS AND CONFERENCES AS NEEDED. 6) RESULTS WILL BE ANALYZED, SHARED AMONG THE PIS AND PREPARED FOR REFEREED PUBLICATIONS. DELIVERABLES: WILL INVESTIGATE THE DEVELOPMENT OF THE REAL NP-FE TEXTURE THROUGH PRECIPITATION OF METALLIC FE FROM A VAPOR PHASE CONSISTING OF SUPERSATURATED FE IN A SILICA-RICH GAS FORMED BY FLASH MELTING OF APPROPRIATE COMPOSITIONS. THIS WILL BE CONDUCTED IN A LAB AT OAK RIDGE NATIONAL LABORATORY. IN ADDITION TO THE ABOVE STUDY, WE WILL PERFORM ADDITIONAL STUDIES ON THE PARTICLE SIZE FRACTION OF THE SOILS <I UM, IN PARTICULAR THE SHAPE PARAMETERS AND THE ARRAYS OF NP-FE ON RIMS AND IN THE AGGLUTINITIC GLASS. THIS WILL BE PERFORMED USING SEM AND TEM INSTRUMENTS IN THE SCIENCE AND ENGINEERING RESEARCH FACILITY, ADJOINING THE EARTH & PLANETARY SCIENCES BUILDING AT THE UNIVERSITY OF TENNESSEE AT KNOXVILLE (THE HORNE INSTITUTION OF THE LEAD INVESTIGATOR FOR THIS TASK).
THE PROPOSAL SEEKS TO MEASURE OXIDATION STATE AND H GRADIENTS IN PRISTINE AND PREVIOUSLY STUDIED LUNAR VOLCANIC GLASS BEADS USING X-RAY ABSORPTION SPECTROSCOPY (XAS) TO MEASURE FE, TI, CR, V, AND EU VALENCE STATES AND QUANTIFY INTRINSIC OXYGEN FUGACITY (FO2). WE WILL CORRELATE OUR RESULTS WITH ATTENUATED TOTAL REFLECTION (ATR) H MAPS ON THE SAME BEADS. RESULTS WILL CONSTRAIN CHEMICAL CHANGES THAT MAY HAVE TAKEN PLACE UNDER TERRESTRIAL CONDITIONS. WE WILL: 1. MEASURE REDOX RATIOS AND DERIVE FO2 IN LUNAR VOLCANIC GLASS BEADS. 2. MAP MULTIVALENT REDOX RATIOS IN LUNAR VOLCANIC GLASS BEADS TO ASSESS LUNAR ERUPTIVE MECHANISMS RECORDED IN LUNAR GLASS BEADS. 3. COMPARE REDOX RATIOS, GRADIENTS, AND DERIVED FO2 IN SURFACE SAMPLES VS. THOSE FROM THE DEEPER REGOLITH (FROM TRENCHES AND CORES) AND IN PRISTINE VS. PREVIOUSLY RELEASED LUNAR GLASSES TO HELP INTERPRET OF LUNAR INTERIOR OXYGEN FUGACITY. 4. COMPARE REDOX RATIOS, GRADIENTS, AND DERIVED FO2 TO HYDROGEN GRADIENTS (I.E., HYDROGEN VS. ELECTRON DIFFUSION) TO INFORM OUR UNDERSTANDING OF BOTH PRE-AND POST-ERUPTIVE MECHANISMS IN LUNAR IGNEOUS MATERIALS AND THE LUNAR INTERIOR. CO-I MCCANTA IS AN EXPERIMENTAL PETROLOGIST WHO HAS PUBLISHED EXTENSIVELY ON THE EFFECTS OF MAGMATIC FO2. SHE WILL BE RESPONSIBLE FOR SUPERVISING THE GRADUATE STUDENT UNDERTAKING INITIAL SAMPLE CHARACTERIZATION NECESSARY TO COMPLETE THE ABOVE TASKS. IN ADDITION, CO-I MCCANTA WILL AID IN OBTAINING AND INTERPRETING THE XAS DATA COLLECTED IN TASKS 1-3. SHE WILL ALSO BE RESPONSIBLE FOR ORGANIZING AND HELPING WRITE THE PROPOSED MANUSCRIPTS.
RESEARCHER TO DEVISE AND COORDINATE SEVERAL SERIES OF PISTON CYLINDER EXPERIMENTS.
THIS STATEMENT OF WORK DESCRIBES THE DUTIES OF THE CHAIR OF THE MAPPING AND PLANETARY SPATIAL INFRASTRUCTURE TEAM (MAPSIT) ADVISORY GROUP. REQUIRED TASKS FOR THE ROLE AS CHAIR INCLUDE PLANNING AND CONDUCTING AN ANNUAL MEETING, PREPARING FOR AND LEADING QUARTERLY STEERING COMMITTEE MEETINGS, PREPARING FOR AND ATTENDING THREE ANNUAL PAC MEETINGS, PREPARING FOR AND HOLDING AN ANNUAL TOWN HALL MEETING, AND ATTENDING TO ROUTINE AS WELL AS URGENT MAPSIT COMMUNICATIONS. 1. PERSONNEL: THE DUTIES DESCRIBED IN THIS SOW WILL BE EXECUTED BY THE PROJECT PI, BRADLEY THOMSON (EPS DEPT.), IN HIS ROLE AS CHAIR OF THE OF THE MAPPING AND PLANETARY SPATIAL INFRASTRUCTURE TEAM (MAPSIT) ADVISORY GROUP. 2. OBJECTIVES: REQUIRED TASKS FOR THE ROLE AS CHAIR INCLUDE PLANNING AND CONDUCTING AN ANNUAL MEETING, PREPARING FOR AND LEADING QUARTERLY STEERING COMMITTEE MEETINGS, PREPARING FOR AND ATTENDING ANNUAL PAC MEETINGS, PREPARING FOR AND HOLDING AN ANNUAL TOWN HALL MEETING, AND ATTENDING TO ROUTINE AS WELL AS URGENT MAPSIT COMMUNICATIONS. 3. TIMELINE: THE PERIOD OF PERFORMANCE FOR THIS SOW IS JAN 3 TO OCT 25, 2022. 4. LOCATION: WORK WILL BE CONDUCTED AT THE PI"S HOST INSTITUTION OF THE UNIVERSITY OF TENNESSEE. 5. DELIVERABLES: THE GOAL OF THE THIS ADVISORY GROUP (AG) IS SIMILAR TO THE OTHER NASA AGS: TO COLLECT AND PRIORITIZE ISSUES OF CONCERN TO THE PLANETARY COMMUNITY THAT INVOLVE PLANETARY DATA INFRASTRUCTURE. THEREFORE, THE MAIN DELIVERABLE IS TIMELY AND EFFECTIVE COMMUNICATION BETWEEN THE COMMUNITY AND NASA.
Lunar awards as prime
| Award | Description | Period | Obligated |
|---|---|---|---|
| 80NSSC20K1055 | SCIENCE GOALS AND OBJECTIVES: THIS PROPOSAL IS FOR A THREE-YEAR PERIOD TO REPROCESS THE MONOSTATIC RADAR DATA OF THE MOON ACQUIRED BY THE MINI-RF INSTRUMENT ON THE LUNAR RECONNAISSANCE ORBITER. | 2020-05-07 → 2025-05-06 | $395K |
| NNX17AL07G | THE EMERGENCE OF OXYGEN AND THE EVOLUTION OF PLANETARY INTERIORS ARE RECORDED IN THE REDOX STATES OF MULTIVALENT ELEMENTS (FE TI MN CR V AND EU) THAT ARE LOCKED IN ROCKS AND THE GLASSES AND MINERALS THAT CONSTITUTE THEM ON PLANETARY SURFACES. AS RECORDERS OF FORMATION CONDITIONS GLASSES AND AMORPHOUS MATERIALS COMPRISE MAJOR CONSTITUENTS OF PLANETARY MATERIALS ON BODIES WHERE MAGMATISM AND/OR IMPACT PROCESSES OCCUR. GLASS IS COMMON IN STONY METEORITES (BOTH ACHONDRITES AND CHONDRITES) AND LUNAR SAMPLES AND IS LIKELY TO BE PRESENT IN SAMPLES RETURNED FROM ASTEROIDS AND PLANETARY SURFACES SUCH AS BENNU (TARGET OF OSIRIS-REX) AND MARS. ROBUST LABORATORY ANALYSES OF MULTIVALENT ELEMENT REDOX STATES IN GLASSES FROM METEORITES AND RETURNED EXTRATERRESTRIAL MATERIALS ARE THUS ESSENTIAL TO FACILITATE UNDERSTANDING OF THE ROLE OF OXYGEN IN SOLAR SYSTEM PROCESSES. HOWEVER INTERPRETABLE MEASUREMENTS OF REDOX STATES AT SUB-NM AND PM SCALES STILL PRESENT FORMIDABLE ANALYTICAL CHALLENGES DUE TO THE LACK OF SUITABLE CALIBRATION SAMPLES. OUR GROUP HAS ALREADY DEVELOPED AN INTERNATIONALLY-USED SET OF CALIBRATION SAMPLES/SOFTWARE FOR X-RAY ABSORPTION SPECTROSCOPY (XAS) MEASUREMENTS OF FE REDOX STATES IN GARNETS AND AMPHIBOLES AS WELL AS IN A SELECT RANGE OF TERRESTRIALLY-RELEVANT SILICATE GLASS COMPOSITIONS. THIS PROPOSAL SEEKS TO BROADEN OUR GLASS CALIBRATION TO INCLUDE OTHER TRANSITION METALS (TI MN CR V AND EU) AND COVER THE REDUCED OXYGEN FUGACITIES NEEDED TO REPRESENT THE DIVERSITY OF SOLAR SYSTEM MATERIALS. SUCH DEVELOPMENT OF THE CAPABILITY TO MEASURE IN SITU REDOX STATES AT ATOMIC AND NEAR-ATOMIC LEVELS IN GLASSES HAS THE POTENTIAL TO MAKE DRAMATIC ADVANCES IN THE STUDY OF SOLAR SYSTEM MATERIALS IN BOTH RETURNED SAMPLES AND METEORITES. THEREFORE THIS PROPOSAL SEEKS TO CREATE A BROAD SUITE OF GLASSES OF GEOLOGICAL RELEVANCE FOR USE AS STANDARDS IN XAS CALIBRATIONS FOR THE STUDY OF EXTRATERRESTRIAL GLASS SAMPLES. USING SYNTHESIZED SAMPLES EQUILIBRATED OVER A RANGE OF OXYGEN FUGACITIES REPRESENTING THOSE FOUND IN OUR SOLAR SYSTEM WE WILL GENERATE XAS CALIBRATION DATA FOR REDOX CALIBRATIONS OF FE TI MN CR V AND EU IN GLASSES THAT ARE DIRECTLY REPRESENTATIVE OF OBSERVED METEORITIC AND PLANETARY COMPOSITIONS. WE WILL MAKE THESE ALIBRATIONS AVAILABLE TO THE PLANETARY MATERIALS AND BROADER SCIENCE COMMUNITIES VIA DISTRIBUTION DIRECTLY TO ALL INTERNATIONAL SYNCHROTRON FACILITIES WITH SPECTRAL DATA POSTED ON THE PDS GEOSCIENCES SPECTRAL LIBRARY. THE TASKS ARE AS FOLLOWS: 1) SYNTHESIZE GLASSES OVER A WIDE RANGE OF GEOLOGICALLY-RELEVANT CHEMICAL BULK COMPOSITIONS AT SEVERAL FO2 S USING A RANGE OF NATURALLYOCCURRING ABUNDANCES FOR FE AND DOPING OF OTHER MULTIVALENT SPECIES INCLUDING V TI EU MN AND CR. 2) CHARACTERIZE THE REDOX CONTENT OF EACH GLASS RELATIVE TO COMPOSITION AND FO2 USING M SSBAUER FOR FE AND ION MICROPROBE FOR EU AND XAS TECHNIQUES FOR FE V TI EU MN AND CR. 3) USE THOSE DATA TO BUILD A STATISTICAL MODEL FOR MEASURING REDOX RATIOS FOR EU AND FE (WHERE WE HAVE INDEPENDENT MEASUREMENTS) AND DIRECTLY PREDICTING OXYGEN FUGACITY FOR EACH OF THESE CATIONS ACROSS OUR BROAD COMPOSITIONAL RANGE USING SOPHISTICATED MULTIVARIATE ANALYSIS TECHNIQUES. THIS WORK IS HIGHLY RELEVANT TO NASA S PDART PROGRAM AS IT WILL GENERATE VALUABLE NEW REFERENCE INFORMATION (LABORATORY SAMPLES AND XAS MEASUREMENTS) AND DEVELOP HIGH-ORDER SOFTWARE FOR PREDICTING VALENCE STATE. THE LATTER TOOLS WILL ENABLE USE OF THE XAS TECHNIQUE TO PRODUCE REDOX STATE MEASUREMENTS OF FE TI MN CR V AND EU WITH KNOWN ACCURACY FOR A WIDE RANGE OF EXTRATERRESTRIALLY-RELEVANT GLASS COMPOSITIONS. OUR DELIVERABLES WILL ENSURE THAT MICROANALYSIS OF REDOX STATES CAN BE USED BROADLY BY THE PLANETARY COMMUNITY TO MAXIMIZE SCIENCE RETURN FROM PRECIOUS EXTRATERRESTRIAL SAMPLES. | 2017-05-16 → 2023-05-15 | $347K |
| NNX17AG15G | WE PROPOSE TO OBSERVE THE CLASSICAL URANIAN SATELLITES MIRANDA ARIEL UMBRIEL TITANIA AND OBERON TO CONSTRAIN THE COMPOSITION AND DISTRIBUTION OF CONSTITUENTS ON THEIR SURFACES. BY MAPPING THE COMPOSITION OF THE URANIAN SATELLITES AND CHARACTERIZING THE SPECTRAL PROPERTIES OF DETECTED CONSTITUENTS WE WILL INVESTIGATE THE PROCESSES MODIFYING THE SURFACES OF THESE MOONS. THE URANIAN MOONS ARE PRIMARILY COMPOSED OF WATER ICE MIXED WITH DARK POTENTIALLY CARBONACEOUS MATERIAL. CARBON DIOXIDE ICE HAS ALSO BEEN DETECTED PRIMARILY ON THE TRAILING HEMISPHERES OF THESE TIDALLY-LOCKED MOONS AND PRIMARILY ON THE MOONS CLOSEST TO URANUS. WATER ICE BANDS ARE STRONGER ON THE LEADING HEMISPHERES OF THESE MOONS WITH THE LEADING/TRAILING ASYMMETRY IN BAND STRENGTH DECREASING WITH DISTANCE FROM URANUS. SIMILARLY THE LEADING HEMISPHERES OF THESE MOONS ARE SPECTRALLY REDDER THAN THEIR TRAILING HEMISPHERES WITH THE DEGREE OF REDDENING INCREASING WITH DISTANCE FROM URANUS. OUR PREFERRED HYPOTHESES TO EXPLAIN THE OBSERVED CONSTITUENT DISTRIBUTIONS ARE THAT MAGNETOSPHERICALLY-EMBEDDED CHARGED PARTICLE BOMBARDMENT AND MICROMETEORITE IMPACTS ARE PRIMARILY MODIFYING THE TRAILING AND LEADING HEMISPHERES OF THESE MOONS RESPECTIVELY. PREVIOUS OBSERVATIONS OF THESE MOONS ARE GENERALLY CONSISTENT WITH THESE COMPLEMENTARY HYPOTHESES BUT NOTABLE MYSTERIES REGARDING THE DISTRIBUTION OF CONSTITUENTS ON THESE MOONS STILL REMAIN. OVER THE LAST DECADE NEAR-INFRARED OBSERVATIONS HAVE DETECTED THE CARBON DIOXIDE COMBINATION AND OVERTONE BANDS BETWEEN 1.9 AND 2.1 MICRONS; HOWEVER THE SIGNIFICANTLY STRONGER CARBON DIOXIDE ASYMMETRIC STRETCH FUNDAMENTAL BAND (CENTERED NEAR 4.27 MICRONS) HAS NOT BEEN DETECTED. ALTHOUGH CARBON DIOXIDE ABUNDANCE IS GREATER ON THE MOONS CLOSE TO URANUS (ARIEL AND UMBRIEL) COMPARED TO THE OUTER SATELLITES (TITANIA AND OBERON) THERE HAS BEEN NO DETECTION OF CARBON DIOXIDE ON THE INNERMOST CLASSICAL MOON MIRANDA. FURTHERMORE WATER ICE BAND STRENGTHS APPEAR TO BE INVERTED ON MIRANDA WITH STRONGER WATER ICE BANDS ON ITS TRAILING HEMISPHERE. RECENT OBSERVATIONS BY OUR TEAM CONFIRM THAT THE OUTER MOONS TITANIA AND OBERON ARE SPECTRALLY REDDER THAN THE INNER MOONS BUT OUR DATA SUGGEST THAT TITANIA IS SPECTRALLY REDDER THAN THE FURTHEST CLASSICAL MOON OBERON UNLIKE PREVIOUS ANALYSES MADE USING DATA COLLECTED BY VOYAGER 2. WE ALSO DETECT CLEAR LATITUDINAL TRENDS IN WATER ICE BAND STRENGTHS ON THESE MOONS WITH STRONGER WATER ICE BANDS ON THEIR CURRENTLY OBSERVABLE NORTHERN HEMISPHERES COMPARED TO OBSERVATIONS MADE PREVIOUSLY OVER THEIR SOUTHERN HEMISPHERES. NEAR-INFRARED SPECTRA OF BOTH MIRANDA AND ARIEL INCLUDE POTENTIAL HINTS OF AMMONIA-HYDRATE FEATURES BETWEEN 2.2 AND 2.3 MICRONS BUT THE POOR QUALITY OF THESE DATA LIMIT ANALYSES REQUIRING HIGHER SIGNAL-TO-NOISE FOLLOW UP OBSERVATIONS. THUS THE DISTRIBUTION OF CONSTITUENTS ON THE CLASSICAL URANIAN SATELLITES IS STILL POORLY UNDERSTOOD WITH MANY MYSTERIES LEFT TO EXPLORE. IN ORDER TO INVESTIGATE THE COMPOSITIONS AND DISTRIBUTION OF MATERIALS ON THESE MOONS WE PROPOSE TO: * GATHER VISIBLE AND NEAR-INFRARED SPECTRA. * MEASURE CONSTITUENT BAND DEPTHS AND AREAS. * MEASURE SPECTRAL SLOPES. * CHARACTERIZE HEMISPHERICAL TRENDS IN THE DISTRIBUTION OF CONSTITUENTS * USE SPECTRAL MODELING CODES TO CONSTRAIN THE GRAIN SIZE AND MIXING REGIMES OF DETECTED CONSTITUENTS. * WITH MINOR ADDITIONAL EFFORT WE WILL USE THESE OBSERVATIONS MEASUREMENTS AND MODELING CODES TO CONSTRAIN THE COMPOSITION OF THE DARK AND POTENTIALLY C-RICH MATERIAL. THE GOALS OF THIS PROJECT ARE WELL ALIGNED WITH NASA S PLANETARY SCIENCE OBJECTIVES IN THE OUTER SOLAR SYSTEM WHICH INCLUDES INVESTIGATION OF THE PROCESS MODIFYING THE SURFACES OF THE CLASSICAL URANIAN MOONS CONSTRAINING POTENTIAL SOURCES OF ORGANIC MATERIAL AND EXPLORING BODIES THAT COULD BE OCEAN WORLDS WITH SUBSURFACE LIQUID LAYERS. | 2017-06-01 → ? | $230K |
| NNX17AI80G | SCIENCE GOALS AND OBJECTIVES: THE GOAL OF THE PROPOSED STUDY IS TO USE METER-TODECAMETER- RESOLUTION TOPOGRAPHY AND RADAR DATA TO EXAMINE CRATERS ON THE MOON WITH THE OBJECTIVES OF: (1) CONSTRAINING THE RATES AND PROCESSES LEADING TO CRATER DEGRADATION AND TOPOGRAPHIC EVOLUTION ON THE MOON (2) USING VARIATIONS IN FRESH CRATER MORPHOMETRY TO EXPLORE PHYSICAL CHARACTERISTICS OF THE CRUST AND REGOLITH AND (3) COMPARING RADAR PROPERTIES AND TOPOGRAPHIC CHARACTERISTICS OF CRATERS IN A RANGE OF DEGRADATION STATES TO EXPLORE REGOLITH EVOLUTION IN RESPONSE TO IMPACT GARDENING. METHODOLOGY: WE PROPOSE TO MAKE NEW MEASUREMENTS OF THE TOPOGRAPHY OF CRATERS ON HIGHLANDS SURFACES TO ASSESS WHETHER THE DEGRADATION SEQUENCE FOR THE MARIA IS CONSISTENT WITH MEASUREMENTS IN THE HIGHLANDS. SECOND WE PROPOSE FURTHER TESTS OF THE LINEAR DIFFUSION MODEL FOR CRATER DEGRADATION TO DETERMINE IF THERE IS SOME SCALE-DEPENDENCE OR NON-LINEARITY IN THE WAY LUNAR TOPOGRAPHY EVOLVES THAT NEEDS FURTHER CHARACTERIZATION. SPECIFICALLY BY MEASURING THE TOPOGRAPHY AND CRATER STATISTICS IN SATURATION (FOR D ~10 TO 200 M DIAMETER CRATERS) WE CAN TEST WHETHER THE KM-SCALE DIFFUSION RATE IS RECONCILABLE WITH THE EVOLUTION OF SMALLER FEATURES. THIRD WE WILL USE MINI-RF RADAR MEASUREMENTS OF LUNAR CRATERS THAT HAVE DISTINCTIVE RADAR HALOS TO ASSESS HOW THE RADAR PROPERTIES CHANGE WITH TIME COMPARED TO THEIR TOPOGRAPHY. CO-I THOMSON WILL LEAD THIS THIRD TASK AND IN ADDITION HE WILL BE AN ACTIVE PARTICIPANT AND CONTRIBUTOR TO THE DATA ANALYSIS INTERPRETATION AND PUBLICATION PREPARATION AS PART OF ALL OTHER TASKS. | 2017-03-17 → 2021-03-16 | $120K |