Association Of Universities For

CONSTRUCTION OF THE LARGE SYNOPTIC SURVEY TELESCOPE (LSST) UNDER THE MAJOR RESEARCH EQUIPMENT AND FACILITIES CONSTRUCTION (MREFC) ACCOUNT

MANAGEMENT AND OPERATIONS OF THE GEMINI OBSERVATORY

AURA MANAGEMENT AND OPERATION OF THE NATIONAL SOLAR OBSERVATORY

ADVANCED TECHNOLOGY SOLAR TELESCOPE (ATST) CONSTRUCTION UNDER THE MAJOR RESEARCH EQUIPMENT AND FACILITIES CONSTRUCTION (MREFC) ACCOUNT

MANAGEMENT AND OPERATIONS OF THE GEMINI OBSERVATORY

MANAGEMENT AND OPERATIONS OF THE NATIONAL OPTICAL ASTRONOMY OBSERVATORY

MANAGEMENT, OPERATIONS AND MAINTENANCE OF THE INTERNATIONAL GEMINI OBSERVATORY -NSF?S NATIONAL OPTICAL-INFRARED ASTRONOMY RESEARCH LABORATORY (NSF?S NOIRLAB) IS THE U.S. NATIONAL CENTER FOR GROUND-BASED NIGHTTIME OPTICAL ASTRONOMY. NOIRLAB INCLUDES THE INTERNATIONAL GEMINI OBSERVATORY, THE KITT PEAK NATIONAL OBSERVATORY, THE CERRO TOLOLO INTER-AMERICAN OBSERVATORY, OPERATIONS OF VERA C. RUBIN OBSERVATORY, AND THE COMMUNITY SCIENCE AND DATA CENTER (CSDC). THIS AWARD SUPPORTS MANAGEMENT, OPERATIONS AND MAINTENANCE OF THESE FACILITIES FOR FIVE YEARS, 2023-2027. THE AWARD SUPPORTS PREPARATIONS FOR THE LAUNCH OF RUBIN OBSERVATORY AND THE FIRST THREE YEARS OF RUBIN?S TEN-YEAR LEGACY SURVEY IN SPACE AND TIME (LSST). GEMINI IS OPERATED BY NSF IN COLLABORATION WITH ITS INTERNATIONAL PARTNERS IN CANADA, BRAZIL, ARGENTINA, THE REPUBLIC OF KOREA, AND CHILE. RUBIN IS OPERATED JOINTLY WITH THE DEPARTMENT OF ENERGY. NOIRLAB WILL ALSO CONTINUE AND FURTHER DEVELOP AN AMBITIOUS PROGRAM OF COMMUNICATION, EDUCATION, AND OUTREACH ACTIVITIES. NOIRLAB COMMUNICATES THE WONDERS OF ASTRONOMY THROUGH ITS FACILITIES, TECHNOLOGY AND PEOPLE. NOIRLAB ENGAGES WITH THE PUBLIC LOCALLY THROUGH A RANGE OF FACE-TO-FACE ACTIVITIES IN HAWAI?I, CHILE AND ARIZONA, AND ON A NATIONAL AND INDEED INTERNATIONAL LEVEL THROUGH ON-LINE PUBLICATIONS, EDUCATIONAL RESOURCES, AND CITIZEN-SCIENCE PROJECTS. THROUGH ITS TELESCOPES, INSTRUMENTS AND SOFTWARE SERVICES, NOIRLAB SUPPORTS OVER 400 GRADUATE THESIS PROJECTS AND OF ORDER 550 NON-THESIS GRADUATE STUDENTS EACH YEAR. ON A YEARLY BASIS, NOIRLAB FACILITIES GENERATE DATA FOR MORE THAN 700 SCIENTIFIC PAPERS. NOIRLAB'S VISION IS TO BE THE PREEMINENT LABORATORY FOR RESEARCH IN MODERN GROUND-BASED OPTICAL-INFRARED (OIR) ASTRONOMY, SUPPORTING A DIVERSE COMMUNITY OF SCIENTISTS SPREAD ACROSS ALL 50 STATES THROUGH THE ENTIRE RESEARCH LIFE CYCLE. NSF?S GOAL IS TO CREATE IN NOIRLAB A NATIONAL RESOURCE THAT WILL LEAD THE WORLD IN DATA-INTENSIVE ASTRONOMY, DRIVE EXPLORATION OF THE NEW FRONTIERS IN TIME-DOMAIN ASTRONOMY AND MULTI-MESSENGER ASTROPHYSICS, MAXIMIZE SCIENCE RETURN FROM RUBIN OBSERVATORY, AND PROVIDE A FOUNDATION FOR ALL U.S. SCIENTISTS TO MAKE FULL USE OF POTENTIAL FUTURE EXTREMELY LARGE TELESCOPES IN THE 2030S AND BEYOND. FOR THE SCIENCE COMMUNITY NOIRLAB PROVIDES ACCESS TO STATE-OF-THE-ART INSTRUMENTATION ON LARGE (8-METER MIRROR DIAMETER) AND MEDIUM-SIZED OR ?MID-SCALE? (APPROXIMATELY 4-METER DIAMETER) OIR TELESCOPES TO ENABLE RESEARCH IN ALL AREAS OF ASTRONOMY. NOIRLAB ALSO PROVIDE A NATIONAL FOCUS FOR THE DEVELOPMENT OF RESEARCH AND EDUCATIONAL PARTNERSHIPS WITH UNIVERSITIES, OTHER NSF-FUNDED RESEARCH DISCIPLINES, OTHER FUNDING AGENCIES, AND INTERNATIONAL COMMUNITIES. OVER THE NEXT FIVE YEARS NOIRLAB WILL CONTINUE TO OPERATE AND DEVELOP THE 4-METER BLANCO AND SOUTHERN ASTROPHYSICAL RESEARCH (SOAR) TELESCOPES IN CHILE AND THE TWIN 8-METER GEMINI TELESCOPES IN HAWAI?I AND CHILE. NOIRLAB WILL SUPPORT PRE-OPERATIONS OF RUBIN LEADING TO COMMISSIONING IN 2024 AND THE LAUNCH OF LSST SHORTLY THEREAFTER. RUBIN WILL UNDOUBTEDLY REVOLUTIONIZE MODERN ASTRONOMY THROUGH ITS EXTENSIVE SURVEY OF THE SOUTHERN SKIES BUT ALSO BY RELEASING MILLIONS OF TIME DOMAIN ALERTS EVERY NIGHT. RUBIN, WORKING IN CONCERT WITH THE OTHER NOIRLAB TELESCOPES AND WITH SOFTWARE AND ARCHIVAL SUPPORT FROM CSDC, WILL HAVE A SIGNIFICANT IMPACT ON ALL OF THE PRIORITY SCIENCE AREAS IDENTIFIED IN THE RECENT NATIONAL ACADEMIES OF SCIENCES, ENGINEERING AND MEDICINE (NASEM) DECADAL SURVEY IN ASTRONOMY AND ASTROPHYSICS, PATHWAYS TO DISCOVERY IN ASTRONOMY & ASTROPHYSICS FOR THE 2020S (ASTRO2020). THIS AWARD REFLECTS NSF'S STATUTORY MISSION AND HAS BEEN DEEMED WORTHY OF SUPPORT THROUGH EVALUATION USING THE FOUNDATION'S INTELLECTUAL MERIT AND BROADER IMPACTS REVIEW CRITERIA.

ADVANCED TECHNOLOGY SOLAR TELESCOPE (ATST) CONSTRUCTION UNDER THE AMERICAN RECOVERY AND REINVESTMENT ACT OF 2009 (ARRA)

MANAGEMENT AND OPERATIONS OF THE NATIONAL OPTICAL ASTRONOMY OBSERVATORY

NSF'S NOIRLAB: MANAGEMENT AND OPERATIONS OF THE DIRECTORATE, MID-SCALE OBSERVATORIES, AND THE COMMUNITY SCIENCE AND DATA CENTER (NOIRLAB BASE) -NSF?S NATIONAL OPTICAL-INFRARED ASTRONOMY RESEARCH LABORATORY (NSF?S NOIRLAB) IS THE U.S. NATIONAL CENTER FOR GROUND-BASED NIGHTTIME OPTICAL ASTRONOMY. NOIRLAB INCLUDES THE INTERNATIONAL GEMINI OBSERVATORY, THE KITT PEAK NATIONAL OBSERVATORY, THE CERRO TOLOLO INTER-AMERICAN OBSERVATORY, OPERATIONS OF VERA C. RUBIN OBSERVATORY, AND THE COMMUNITY SCIENCE AND DATA CENTER (CSDC). THIS AWARD SUPPORTS MANAGEMENT, OPERATIONS AND MAINTENANCE OF THESE FACILITIES FOR FIVE YEARS, 2023-2027. THE AWARD SUPPORTS PREPARATIONS FOR THE LAUNCH OF RUBIN OBSERVATORY AND THE FIRST THREE YEARS OF RUBIN?S TEN-YEAR LEGACY SURVEY IN SPACE AND TIME (LSST). GEMINI IS OPERATED BY NSF IN COLLABORATION WITH ITS INTERNATIONAL PARTNERS IN CANADA, BRAZIL, ARGENTINA, THE REPUBLIC OF KOREA, AND CHILE. RUBIN IS OPERATED JOINTLY WITH THE DEPARTMENT OF ENERGY. NOIRLAB WILL ALSO CONTINUE AND FURTHER DEVELOP AN AMBITIOUS PROGRAM OF COMMUNICATION, EDUCATION, AND OUTREACH ACTIVITIES. NOIRLAB COMMUNICATES THE WONDERS OF ASTRONOMY THROUGH ITS FACILITIES, TECHNOLOGY AND PEOPLE. NOIRLAB ENGAGES WITH THE PUBLIC LOCALLY THROUGH A RANGE OF FACE-TO-FACE ACTIVITIES IN HAWAI?I, CHILE AND ARIZONA, AND ON A NATIONAL AND INDEED INTERNATIONAL LEVEL THROUGH ON-LINE PUBLICATIONS, EDUCATIONAL RESOURCES, AND CITIZEN-SCIENCE PROJECTS. THROUGH ITS TELESCOPES, INSTRUMENTS AND SOFTWARE SERVICES, NOIRLAB SUPPORTS OVER 400 GRADUATE THESIS PROJECTS AND OF ORDER 550 NON-THESIS GRADUATE STUDENTS EACH YEAR. ON A YEARLY BASIS, NOIRLAB FACILITIES GENERATE DATA FOR MORE THAN 700 SCIENTIFIC PAPERS. NOIRLAB'S VISION IS TO BE THE PREEMINENT LABORATORY FOR RESEARCH IN MODERN GROUND-BASED OPTICAL-INFRARED (OIR) ASTRONOMY, SUPPORTING A DIVERSE COMMUNITY OF SCIENTISTS SPREAD ACROSS ALL 50 STATES THROUGH THE ENTIRE RESEARCH LIFE CYCLE. NSF?S GOAL IS TO CREATE IN NOIRLAB A NATIONAL RESOURCE THAT WILL LEAD THE WORLD IN DATA-INTENSIVE ASTRONOMY, DRIVE EXPLORATION OF THE NEW FRONTIERS IN TIME-DOMAIN ASTRONOMY AND MULTI-MESSENGER ASTROPHYSICS, MAXIMIZE SCIENCE RETURN FROM RUBIN OBSERVATORY, AND PROVIDE A FOUNDATION FOR ALL U.S. SCIENTISTS TO MAKE FULL USE OF POTENTIAL FUTURE EXTREMELY LARGE TELESCOPES IN THE 2030S AND BEYOND. FOR THE SCIENCE COMMUNITY NOIRLAB PROVIDES ACCESS TO STATE-OF-THE-ART INSTRUMENTATION ON LARGE (8-METER MIRROR DIAMETER) AND MEDIUM-SIZED OR ?MID-SCALE? (APPROXIMATELY 4-METER DIAMETER) OIR TELESCOPES TO ENABLE RESEARCH IN ALL AREAS OF ASTRONOMY. NOIRLAB ALSO PROVIDE A NATIONAL FOCUS FOR THE DEVELOPMENT OF RESEARCH AND EDUCATIONAL PARTNERSHIPS WITH UNIVERSITIES, OTHER NSF-FUNDED RESEARCH DISCIPLINES, OTHER FUNDING AGENCIES, AND INTERNATIONAL COMMUNITIES. OVER THE NEXT FIVE YEARS NOIRLAB WILL CONTINUE TO OPERATE AND DEVELOP THE 4-METER BLANCO AND SOUTHERN ASTROPHYSICAL RESEARCH (SOAR) TELESCOPES IN CHILE AND THE TWIN 8-METER GEMINI TELESCOPES IN HAWAI?I AND CHILE. NOIRLAB WILL SUPPORT PRE-OPERATIONS OF RUBIN LEADING TO COMMISSIONING IN 2024 AND THE LAUNCH OF LSST SHORTLY THEREAFTER. RUBIN WILL UNDOUBTEDLY REVOLUTIONIZE MODERN ASTRONOMY THROUGH ITS EXTENSIVE SURVEY OF THE SOUTHERN SKIES BUT ALSO BY RELEASING MILLIONS OF TIME DOMAIN ALERTS EVERY NIGHT. RUBIN, WORKING IN CONCERT WITH THE OTHER NOIRLAB TELESCOPES AND WITH SOFTWARE AND ARCHIVAL SUPPORT FROM CSDC, WILL HAVE A SIGNIFICANT IMPACT ON ALL OF THE PRIORITY SCIENCE AREAS IDENTIFIED IN THE RECENT NATIONAL ACADEMIES OF SCIENCES, ENGINEERING AND MEDICINE (NASEM) DECADAL SURVEY IN ASTRONOMY AND ASTROPHYSICS, PATHWAYS TO DISCOVERY IN ASTRONOMY & ASTROPHYSICS FOR THE 2020S (ASTRO2020). THIS AWARD REFLECTS NSF'S STATUTORY MISSION AND HAS BEEN DEEMED WORTHY OF SUPPORT THROUGH EVALUATION USING THE FOUNDATION'S INTELLECTUAL MERIT AND BROADER IMPACTS REVIEW CRITERIA.

NSF'S NATIONAL OPTICAL-INFRARED ASTRONOMY RESEARCH LABORATORY (NOIRLAB): MANAGEMENT AND OPERATIONS OF VERA C. RUBIN OBSERVATORY -NSF?S NATIONAL OPTICAL-INFRARED ASTRONOMY RESEARCH LABORATORY (NSF?S NOIRLAB) IS THE U.S. NATIONAL CENTER FOR GROUND-BASED NIGHTTIME OPTICAL ASTRONOMY. NOIRLAB INCLUDES THE INTERNATIONAL GEMINI OBSERVATORY, THE KITT PEAK NATIONAL OBSERVATORY, THE CERRO TOLOLO INTER-AMERICAN OBSERVATORY, OPERATIONS OF VERA C. RUBIN OBSERVATORY, AND THE COMMUNITY SCIENCE AND DATA CENTER (CSDC). THIS AWARD SUPPORTS MANAGEMENT, OPERATIONS AND MAINTENANCE OF THESE FACILITIES FOR FIVE YEARS, 2023-2027. THE AWARD SUPPORTS PREPARATIONS FOR THE LAUNCH OF RUBIN OBSERVATORY AND THE FIRST THREE YEARS OF RUBIN?S TEN-YEAR LEGACY SURVEY IN SPACE AND TIME (LSST). GEMINI IS OPERATED BY NSF IN COLLABORATION WITH ITS INTERNATIONAL PARTNERS IN CANADA, BRAZIL, ARGENTINA, THE REPUBLIC OF KOREA, AND CHILE. RUBIN IS OPERATED JOINTLY WITH THE DEPARTMENT OF ENERGY. NOIRLAB WILL ALSO CONTINUE AND FURTHER DEVELOP AN AMBITIOUS PROGRAM OF COMMUNICATION, EDUCATION, AND OUTREACH ACTIVITIES. NOIRLAB COMMUNICATES THE WONDERS OF ASTRONOMY THROUGH ITS FACILITIES, TECHNOLOGY AND PEOPLE. NOIRLAB ENGAGES WITH THE PUBLIC LOCALLY THROUGH A RANGE OF FACE-TO-FACE ACTIVITIES IN HAWAI?I, CHILE AND ARIZONA, AND ON A NATIONAL AND INDEED INTERNATIONAL LEVEL THROUGH ON-LINE PUBLICATIONS, EDUCATIONAL RESOURCES, AND CITIZEN-SCIENCE PROJECTS. THROUGH ITS TELESCOPES, INSTRUMENTS AND SOFTWARE SERVICES, NOIRLAB SUPPORTS OVER 400 GRADUATE THESIS PROJECTS AND OF ORDER 550 NON-THESIS GRADUATE STUDENTS EACH YEAR. ON A YEARLY BASIS, NOIRLAB FACILITIES GENERATE DATA FOR MORE THAN 700 SCIENTIFIC PAPERS. NOIRLAB'S VISION IS TO BE THE PREEMINENT LABORATORY FOR RESEARCH IN MODERN GROUND-BASED OPTICAL-INFRARED (OIR) ASTRONOMY, SUPPORTING A DIVERSE COMMUNITY OF SCIENTISTS SPREAD ACROSS ALL 50 STATES THROUGH THE ENTIRE RESEARCH LIFE CYCLE. NSF?S GOAL IS TO CREATE IN NOIRLAB A NATIONAL RESOURCE THAT WILL LEAD THE WORLD IN DATA-INTENSIVE ASTRONOMY, DRIVE EXPLORATION OF THE NEW FRONTIERS IN TIME-DOMAIN ASTRONOMY AND MULTI-MESSENGER ASTROPHYSICS, MAXIMIZE SCIENCE RETURN FROM RUBIN OBSERVATORY, AND PROVIDE A FOUNDATION FOR ALL U.S. SCIENTISTS TO MAKE FULL USE OF POTENTIAL FUTURE EXTREMELY LARGE TELESCOPES IN THE 2030S AND BEYOND. FOR THE SCIENCE COMMUNITY NOIRLAB PROVIDES ACCESS TO STATE-OF-THE-ART INSTRUMENTATION ON LARGE (8-METER MIRROR DIAMETER) AND MEDIUM-SIZED OR ?MID-SCALE? (APPROXIMATELY 4-METER DIAMETER) OIR TELESCOPES TO ENABLE RESEARCH IN ALL AREAS OF ASTRONOMY. NOIRLAB ALSO PROVIDE A NATIONAL FOCUS FOR THE DEVELOPMENT OF RESEARCH AND EDUCATIONAL PARTNERSHIPS WITH UNIVERSITIES, OTHER NSF-FUNDED RESEARCH DISCIPLINES, OTHER FUNDING AGENCIES, AND INTERNATIONAL COMMUNITIES. OVER THE NEXT FIVE YEARS NOIRLAB WILL CONTINUE TO OPERATE AND DEVELOP THE 4-METER BLANCO AND SOUTHERN ASTROPHYSICAL RESEARCH (SOAR) TELESCOPES IN CHILE AND THE TWIN 8-METER GEMINI TELESCOPES IN HAWAI?I AND CHILE. NOIRLAB WILL SUPPORT PRE-OPERATIONS OF RUBIN LEADING TO COMMISSIONING IN 2024 AND THE LAUNCH OF LSST SHORTLY THEREAFTER. RUBIN WILL UNDOUBTEDLY REVOLUTIONIZE MODERN ASTRONOMY THROUGH ITS EXTENSIVE SURVEY OF THE SOUTHERN SKIES BUT ALSO BY RELEASING MILLIONS OF TIME DOMAIN ALERTS EVERY NIGHT. RUBIN, WORKING IN CONCERT WITH THE OTHER NOIRLAB TELESCOPES AND WITH SOFTWARE AND ARCHIVAL SUPPORT FROM CSDC, WILL HAVE A SIGNIFICANT IMPACT ON ALL OF THE PRIORITY SCIENCE AREAS IDENTIFIED IN THE RECENT NATIONAL ACADEMIES OF SCIENCES, ENGINEERING AND MEDICINE (NASEM) DECADAL SURVEY IN ASTRONOMY AND ASTROPHYSICS, PATHWAYS TO DISCOVERY IN ASTRONOMY & ASTROPHYSICS FOR THE 2020S (ASTRO2020). THIS AWARD REFLECTS NSF'S STATUTORY MISSION AND HAS BEEN DEEMED WORTHY OF SUPPORT THROUGH EVALUATION USING THE FOUNDATION'S INTELLECTUAL MERIT AND BROADER IMPACTS REVIEW CRITERIA.

COOPERATIVE AGREEMENT FOR THE MANAGEMENT, OPERATION AND THE MAINTENANCE OF THE NATIONAL OPTICAL ASTRONOMY OBSERVATORIES (NOAO)

THE SPACE TELESCOPE SCIENCE INSTITUTE, LEADING AN INSTITUTIONAL PARTNERSHIP WITH THE CHANDRA X-RAY CENTER, THE INFRARED PROCESSING AND ANALYSIS CENTE

MANAGEMENT AND OPERATIONS OF THE NATIONAL SOLAR OBSERVATORY

SUPPORT OF THE MANAGEMENT, OPERATIONS, AND THE MAINTENANCE OF THE NATIONAL SOLAR OBSERVATORY (NSO)

GEMINI OBSERVATORY IN THE ERA OF MULTI-MESSENGER ASTRONOMY: HIGH IMAGE QUALITY AND RAPID RESPONSE TO COSMIC EVENTS

DEVELOPMENT OF THE US EXTREMELY LARGE TELESCOPE PROGRAM

RESEARCH INFRASTRUCTURE: MID-SCALE RI-1 (M1:DA): DESIGN OF A NEXT GENERATION GROUND BASED SOLAR OBSERVING NETWORK (NGGONG-DESIGN) -THE SUN IS THE CLOSEST AND MOST IMPORTANT STAR FOR LIFE ON EARTH. UNDERSTANDING THE COMPLEX PHYSICS BEHIND SOLAR ACTIVITY AND DEVELOPING REALISTIC PREDICTIONS OF SPACE WEATHER REQUIRE COMPREHENSIVE AND CONTINUOUS OBSERVATIONS OF THE FULL DISK OVER MANY DECADES. THE CURRENT GLOBAL OSCILLATION NETWORK GROUP (GONG) PROVIDES THE MOST COMPREHENSIVE CONTEXTUAL DATA TO MODEL THE LARGE- SCALE STATE OF THE SUN?S HELIOSPHERE, THE VAST BUBBLE OF IONIZED PARTICLES FORMING THE SOLAR WIND THAT SURROUNDS THE SOLAR SYSTEM. HOWEVER, GONG IS AGING RAPIDLY, AND PROGRESS IN MODELING SOLAR PHENOMENA AND SPACE WEATHER NOW NEEDS NEW SYNOPTIC OBSERVATIONS NOT CURRENTLY AVAILABLE FROM ITS EXISTING FACILITIES. THIS AWARD WILL SUPPORT THE GONG TEAM TO DESIGN A NEXT GENERATION SOLAR OBSERVING NETWORK (NGGONG), TO BE PLACED AT INTERNATIONAL SITES DISTRIBUTED ACROSS LONGITUDES AND WEATHER PATTERNS TO PROVIDE NEARLY CONTINUOUS OBSERVATIONS OF THE SUN FOR MANY YEARS INTO THE FUTURE. THIS DESIGN WILL MAXIMIZE THE USE OF EXISTING INFRASTRUCTURE AND RESOURCES. THE NGGONG DESIGN ACTIVITIES INCLUDE AN INNOVATIVE POST-BACCALAUREATE PROGRAM EXPECTED TO PROVIDE SIGNIFICANT BENEFIT TO THE FUTURE STEM WORKFORCE. A SECOND PROGRAM WILL HELP TO BRIDGE A CRITICAL GAP THAT MANY FIRST-GENERATION STUDENTS FACE BETWEEN UNDERGRADUATE AND GRADUATE LEVELS. NGGONG HAS THE POTENTIAL FOR STRONG PARTNERSHIPS BOTH DOMESTIC AND INTERNATIONAL. NGGONG HAS THE POTENTIAL FOR STRONG PARTNERSHIPS, BOTH DOMESTIC, SUCH AS WITH THE NATIONAL OCEANIC AND ATMOSPHERIC ADMINISTRATION AND THE DEPARTMENT OF DEFENSE, AND INTERNATIONALLY, INCLUDING WITH THE EUROPEAN UNION AND JAPAN. THE FUTURE NGGONG NETWORK WILL PROVIDE A QUANTITATIVE CONTEXT FOR HIGH-RESOLUTION SOLAR AND IN-SITU MEASUREMENTS AND MODELS, BRIDGING SOLAR AND STELLAR RESEARCH IN THE AREA OF STELLAR ACTIVITY AND ITS CONSEQUENCES FOR HABITABILITY ON OUR OWN AND OTHER PLANETS. IT WILL BE A PLATFORM FOR FUTURE INSTRUMENT DEVELOPMENT. NGGONG IS KEY TO MEASURING THE PROCESSES THAT DRIVE ACTIVITY FROM THE SOLAR INTERIOR THROUGH ITS ATMOSPHERE AND INTO THE HELIOSPHERE, LEADING TO SPACE WEATHER, AND WILL BUILD A MULTI-DECADE RECORD OF SOLAR VARIABILITY FOR USE BY FUTURE GENERATIONS OF SCIENTISTS, IN BOTH PREDICTABLE AND UNEXPECTED WAYS. THE NGGONG NETWORK ADDRESSES THE NATIONAL SECURITY AND RESEARCH PRIORITIES OF THE NATIONAL SPACE WEATHER STRATEGY AND ACTION PLAN AND THE PROMOTING RESEARCH AND OBSERVATIONS OF SPACE WEATHER TO IMPROVE THE FORECASTING OF TOMORROW ACT. BUT IT MUST BE DESIGNED FIRST. THIS AWARD REFLECTS NSF'S STATUTORY MISSION AND HAS BEEN DEEMED WORTHY OF SUPPORT THROUGH EVALUATION USING THE FOUNDATION'S INTELLECTUAL MERIT AND BROADER IMPACTS REVIEW CRITERIA.- SUBAWARDS ARE NOT PLANNED FOR THIS AWARD.

THE LARGE SYNOPTIC SURVEY TELESCOPE FINAL DESIGN PHASE

PRE-OPERATIONS OF THE LARGE SYNOPTIC SURVEY TELESCOPE (LSST)

NATIONAL SOLAR OBSERVATORY SCIENCE RESEARCH SUPPORT

SUPPORT FOR THE KITT PEAK NATIONAL OBSERVATORY (KPNO) WIYN 3.5-METER TELESCOPE FACILITY

ENABLING A GIANT SEGMENTED MIRROR TELESCOPE FOR THE UNITED STATES ASTRONOMICAL COMMUNITY

ADMINISTRATION BY NOAO OF THE TELESCOPE SYSTEMS INSTRUMENTATION PROGRAM (TSIP)

COMPLETION OF THE DESIGN AND PROJECT DEVELOPMENT PHASES FOR CONSTRUCTION READINESS OF THE LARGE SYNOPTIC SURVEY TELESCOPE (LSST)

THE MULTI-MISSION ARCHIVE AT SPACE SCIENCE INSTITUTE:

THE MULTI-MISSION ARCHIVE AT SPACE TELESCOPE SCIENCE INSTITUTE (MAST) IS NASA'S ARCHIVE CENTER FOR OPTICAL/UV SPACE ASTROPHYSICS DATA. MAST PROVIDE

SUPPORT FOR THE KITT PEAK NATIONAL OBSERVATORY (KPNO) MAYALL 4-METER TELESCOPE FACILITY

SUPPORT FOR THE KITT PEAK NATIONAL OBSERVATORY (KPNO) WIYN 3.5-METER TELESCOPE FACILITY -MANY STARS IN OUR GALAXY HOST ONE OR MORE PLANETS. WITH THIS AWARD, THE WIYN TELESCOPE AT THE KITT PEAK NATIONAL OBSERVATORY NEAR TUCSON WILL CONTINUE TO BE USED PRIMARILY TO MEASURE THE VELOCITIES AND MASSES OF THESE ?EXOPLANETS?. MASSES ARE NEEDED TO DETERMINE IF AN EXOPLANET IS PRIMARILY GASEOUS, ICY, OR ROCKY. RESEARCH ENABLED BY THIS PROGRAM WILL STRENGTHEN THE FOUNDATIONS FOR IDENTIFYING AND CHARACTERIZING EARTH-LIKE EXOPLANETS IN THE NEARBY COSMOS. THE PRIMARY INSTRUMENT BEING USED AT WIYN, KNOWN AS NEID, EXCEEDS ITS TECHNICAL REQUIREMENTS AND ROUTINELY MEASURES PLANET VELOCITIES TO BETTER THAN A METER PER SECOND. THIS PROPOSAL WILL FUND THE NEXT 45 MONTHS OF NSF?S CONTRIBUTION TO WIYN OPERATIONS, IN SUPPORT OF THE NASA-NSF EXOPLANET OBSERVATIONAL RESEARCH (NN-EXPLORE) PROGRAM. NN-EXPLORE BRINGS TOGETHER FEDERAL AGENCIES, FEDERAL RESEARCH CENTERS, AND U.S. UNIVERSITIES, WITH THE GOAL OF ADVANCING RESEARCH IN EXOPLANETS. THE OPEN ACCESS FOR ENQUIRY-BASED RESEARCH VIA PEER REVIEW AND OPEN DATA FACILITATED BY THIS AWARD WILL ALLOW SCIENTISTS AND CITIZENS TO ENGAGE IN THE WIYN RESEARCH ENTERPRISE NO MATTER WHO THEY ARE OR WHERE THEY WORK. MANY PARTICIPANTS ARE EARLY CAREER SCIENTISTS AND UNDERGRADUATE STUDENTS. UNDER THIS AWARD, NSF?S NATIONAL OPTICAL-INFRARED ASTRONOMY RESEARCH LABORATORY (NOIRLAB) WILL CONTINUE TO OPERATE THE WIYN TELESCOPE FROM 2024 THROUGH 2027 AS NSF?S CONTRIBUTION TO THE NN-EXPLORE PROGRAM. NN-EXPLORE ENABLES SCIENTIFIC RESEARCH RELATED TO THE CHARACTERIZATION OF EXOPLANETS AND THEIR HOST STARS. NEID IS THE ONLY OPEN-ACCESS EXTREME-PRECISION RADIAL VELOCITY INSTRUMENT IN THE U.S. THAT HAS THE TECHNICAL CAPABILITY AND THE REQUIRED YEARS-LONG AND HIGH CADENCE (APPROXIMATELY EVERY OTHER NIGHT) TIME ON SKY TO MEET THE GOAL OF IDENTIFYING NEARBY HABITABLE PLANETS, FOLLOWING UP ON DISCOVERIES BY NASA MISSIONS LIKE KEPLER AND TESS, PICKING KEY TARGETS FOR THE JAMES WEBB AND ROMAN SPACE TELESCOPES, AND BLAZING THE PATH FORWARD TO ENABLE NASA?S FUTURE HABITABLE WORLDS OBSERVATORY. THIS AWARD PROVIDES SUPPORT FOR ESSENTIAL OPERATIONS AND MAINTENANCE OF WIYN, AS WELL AS MINOR TECHNOLOGICAL UPGRADES NEEDED FOR THE CONTINUED OPERATION OF NEID. THIS AWARD REFLECTS NSF'S STATUTORY MISSION AND HAS BEEN DEEMED WORTHY OF SUPPORT THROUGH EVALUATION USING THE FOUNDATION'S INTELLECTUAL MERIT AND BROADER IMPACTS REVIEW CRITERIA.- SUBAWARDS ARE NOT PLANNED FOR THIS AWARD.

INFRASTRUCTURE IMPROVEMENTS AT THE NATIONAL OPTICAL ASTRONOMY OBSERVATORY

ASSOCIATION OF UNIVERSITIES FOR RESEARCH IN ASTRONOMY INC. ASTROPHYSICS SCIENCE EDUCATION AND PUBL

WINDOWS ON THE UNIVERSE CENTER FOR ASTRONOMY OUTREACH (WUCAO)

NCOA TRANSITION PLANNING AND PREPARATION PROJECT

MAST MULTI-MISSION ARCHIVE STSCCL

RENEWING SMALL TELESCOPES FOR ASTRONOMICAL RESEARCH (RESTAR) PHASE 1

JWST TELESCOPE SCIENTIST INVESTIGATION

NSF-NOAA INTERAGENCY AGREEMENT (IAA) FOR THE GLOBAL OSCILLATIONS NETWORK GROUP (GONG) -THIS AWARD IS AN INTERAGENCY AGREEMENT. THIS AWARD REFLECTS NSF'S STATUTORY MISSION AND HAS BEEN DEEMED WORTHY OF SUPPORT THROUGH EVALUATION USING THE FOUNDATION'S INTELLECTUAL MERIT AND BROADER IMPACTS REVIEW CRITERIA.- SUBAWARDS ARE NOT PLANNED FOR THIS AWARD.

FUNDING AUGMENTATION FOR THE DESIGN & DEVELOPMENT PHASE OF THE ADVANCED TECHNOLOGY SOLAR TELESCOPE

THE LARGE SYNOPTIC SURVEY TELESCOPE (LSST) FOR DESIGN AND DEVELOPMENT

INTEGRATING NASA EARTH SCIENCE INTO VIEW SPACE.

THE SEARCH FOR LIFE IS ONE OF THE NEXT GREAT CHALLENGES IN ASTRONOMY. NASA'S 30-YEAR ROADMAP FOR ASTROPHYSICS ENVISIONS A SEARCH FOR SIGNS OF LIFE IN THE ATMOSPHERES OF EARTH-LIKE PLANETS USING SPECTROSCOPY FROM A LARGE SPACE TELESCOPE. NASA IS NOW PURSUING THREE FLAGSHIP CONCEPT STUDIES THAT WILL ENABLE THIS SEARCH (LUVOIR HABEX AND OST). ESTIMATES FOR THE NUMBER OF EARTH-LIKE PLANETS SUCH A MISSION CAN DETECT AND CHARACTERIZE INCREASE AS THE SECOND POWER OF THE APERTURE MOTIVATING TELESCOPES LARGER THAN JWST THAT MUST BE SEGMENTED TO FIT INTO ANTICIPATED LAUNCH FAIRINGS. IT IS CERTAIN THAT A MISSION CAPABLE OF DIRECTLY IMAGING EARTH-LIKE EXOPLANETS WILL INCLUDE A CORONAGRAPH EVEN IF STARSHADES PROVE TO BE EFFECTIVE AND FEASIBLE. THUS THE TECHNOLOGICAL CHALLENGES PRESENTED BY HIGHPERFORMANCE CORONAGRAPHY ON SEGMENTED TELESCOPES MUST BE SOLVED IF WE ARE TO MOUNT A STATISTICALLY ROBUST SEARCH FOR LIFE ON OTHER WORLDS. FOR THREE YEARS OUR GROUP HAS BEEN AT THE FOREFRONT OF DEVELOPING HIGH-PERFORMANCE CORONAGRAPH TECHNOLOGY FOR SEGMENTED APERTURES. WE HAVE BUILT A ROBUST FLEXIBLE TESTBED HICAT FOR OUR APODIZED PUPIL LYOT CORONAGRAPH (APLC) APPROACH TO SEGMENTED APERTURES. BY OPTIMIZING INDIVIDUAL COMPONENTS WE HAVE MATURED THE TECHNOLOGY TO TRL 3. BUT FOR A SEGMENTED TELESCOPE AIMING TO ACHIEVE 1E-10 STARLIGHT SUPPRESSION THE STABILITY OF THE WAVEFRONT DELIVERED FROM THE TELESCOPE PRESENTS SPECIAL CHALLENGES TO CORONAGRAPH PERFORMANCE. THE TELESCOPE AND CORONAGRAPH MUST BE CONSIDERED TOGETHER AND THEIR TECHNOLOGIES ADVANCED AS AN INTEGRATED SYSTEM.

JWST TELESCOPE SCIENTIST INVESTIGATION

DEVELOPING LABORATORY SCALE ACTIVE SEGMENTED TELESCOPES TO ENABLE THE NEXT STAGE OF CORONAGRAPHIC TESTBEDS

THE PI OF THIS PROPOSAL, XXX, WAS APPOINTED AS THE JWST TELESCOPE SCIENTIST IN 2002, IN RESPONSE TO AO 01 OSS 05. THE PRESENT PROPOSAL REQUESTS FUNDI

FACILITY CLASS GUIDE STAR LASER SYSTEMS FOR ASTRONOMICAL ADAPTIVE OPTICS

A KEY CONSEQUENCE OF THESE ADVANCES IS THAT THE CURRENT FRONTIER FOR THEORETICAL GALAXY FORMATION STUDIES LIES WHERE OUR ABILITY TO SIMULATE GALAXIES ENCOMPASSES A FULL TREATMENT OF THE CGM-GALAXY CONNECTION HIGH SPATIAL AND MASS RESOLUTION...

MID-INFRARED SCIENCE WITH THE NEXT GENERATION SPAC E TELESCOPE (NGST): THE STRUCTURE AND MINERALOG

THE SPACE TELESCOPE SCIENCE INSTITUTE (STSCI) IS THE FUTURE HOME OF THE JAMES WEBB SPACE TELESCOPE (JWST) AND HAS BEEN THE HOME INSTITUTION FOR THE H

INFRASTRUCTURE IMPROVEMENTS AT THE NATIONAL SOLAR OBSERVATORY

COLLABORATIVE PROGRAM FOR DEVELOPMENT OF CHILEAN ASTRONOMY

22-SMDSS22-0018 FUNDING DATA ANALYSIS OF JWST GTO OBSERVATIONS BY THE STSCI GROUP

SUPPORT THE HABITABLE WORLDS OBSERVATORY (HWO) SCIENCE SIMULATION TOOLS INSTRUMENT DESIGN AND TESTBED DEVELOPMENT. IT IS NECESSARY TO DEVELOP OR PERFORM 1) THE INITIAL OBSERVATORY ARCHITECTURE S EXPOSURE TIME CALCULATOR AS A COMMUNITY TOOL TO EVALUATE SCIENCE FEASIBILITY FOR GENERAL ASTROPHYSICS 2) A CORONAGRAPH DESIGN IS NEEDED FOR A NEW TELESCOPE TO SUPPORT INTEGRATED MODELING AND PREDICT SCIENCE YIELDS 3) LABORATORY DEMONSTRATIONS OF HIGH CONTRAST POST-PROCESSING APPROACHES AND 4) TESTBED DESIGN IS NEEDED TO SUPPORT TECHNOLOGY MATURATION OF OBSERVATORY SYSTEMS.

PHOTOMETRIC SURVEY OF THE KEPLER TARGET REGION IN RESPONSE TO AO #00-OSS-02, KEPLER DISCOVERY PROGRAM.

EXOPLANET DIRECT IMAGING WITH ON-AXIS SEGMENTED APERTURES IN SPACE WE PROPOSE TO DEVELOP HIGH CONTRAST CORONAGRAPHIC TECHNIQUES FOR SEGMENTED TELESC

SCIENCE GOAL AND OBJECTIVES: WE PROPOSE TO MEASURE THE FLOWS FROM THE SURFACE DOWN TO THE UPPER SHEAR LAYER IN THE CONVECTION ZONE AROUND 5% BELOW THE SURFACE AND PROVIDE OBSERVATIONAL CONSTRAINTS FOR THE LATITUDINAL LONGITUDINAL AND TEMPORAL VARIATIONS OF THE FLOW COMPONENTS. THE GOAL IS TO ESTABLISH THE EXTENT TO WHICH THESE LARGE-SCALE FLOWS DRIVE THE EMERGENCE AND EVOLUTION OF MAGNETIC FLUX AT THE SOLAR SURFACE AND THE SUBSEQUENT POLEWARD FLUX TRANSPORT. THIS WILL LEAD TO A BETTER UNDERSTANDING OF THE GENERATION AND EVOLUTION OF GLOBAL-SCALE MAGNETIC FIELDS. TO ACHIEVE THIS GOAL WE WILL FOCUS ON SURFACE AND SUBSURFACE LARGE-SCALE FLOWS NEAR LOCATIONS OF ACTIVITY INCLUDING ACTIVITY COMPLEXES AND ACTIVE LONGITUDES AND SEARCH FOR SUBSURFACE MARKERS OR EVEN PRECURSORS OF MAGNETIC ACTIVITY. SECOND WE WILL FOCUS ON FLOWS AT MID- TO HIGH LATITUDES WHERE DIFFUSING FLUX IS BEING TRANSPORTED POLEWARD. THIRD WE WILL FOCUS ON THE SOLAR-CYCLE VARIATION OF FLOWS DERIVED FROM LOCATIONS OF HIGH OR LOW ACTIVITY AND THE NORTH-SOUTH ASYMMETRY IN MAGNETIC ACTIVITY AND ITS CONNECTION TO SUBSURFACE FLOWS AND WHETHER THESE FLOWS ARE PRECURSORS OF THE NEXT-CYCLE ACTIVITY. WE WILL STUDY THE FLOWS IN THREE DEPTH RANGES: THE LAYERS CLOSE TO THE SURFACE WHERE THE DENSITY CHANGES BY SEVERAL ORDERS OF MAGNITUDE THE NEAR-SURFACE SHEAR LAYER (NSSL AT ABOUT 35 MM) WHERE THE ROTATION RATE SHOWS A LOCAL MAXIMUM AND THE LAYERS IN BETWEEN THESE TWO. THE FLOWS IN THESE LAYERS HAVE THE MOST DIRECT INFLUENCE ON SURFACE ACTIVITY. METHODOLOGY: WE WILL PERFORM A COMPREHENSIVE STUDY OF THE LARGE-SCALE HORIZONTAL FLOWS (ZONAL AND MERIDIONAL FLOWS) FROM THE SURFACE TO A DEPTH OF ABOUT 40 MM (94% SOLAR RADIUS) FROM THE EQUATOR TO 70 DEGREE LATITUDE OR HIGHER. WE WILL FOCUS ON THEIR VARIATION WITH LATITUDE LONGITUDE AND TIME. WE WILL STUDY THE VARIATION FROM ONE ROTATION TO THE NEXT AND DURING THE COURSE OF A SOLAR CYCLE. TO DERIVE THE SUBSURFACE FLOW COMPONENTS WE WILL APPLY RING-DIAGRAM ANALYSIS (A WELL-ESTABLISHED HELIOSEISMIC TECHNIQUE) TO SDO/ HMI DOPPLERGRAMS. AS A STARTING POINT WE WILL USE THE FLOW VALUES DERIVED FROM THE STANDARD HMI RING-DIAGRAM PIPELINE WITH THREE DIFFERENT TILE SIZES. WE HAVE PREVIOUSLY STUDIED THE SUBSURFACE FLOWS IN THE NEAR-SURFACE LAYERS (TO A DEPTH OF 16 MM) WITH VELOCITIES FROM THE HMI 15-DEGREE RING-DIAGRAM PIPELINE. FOR THE PROPOSED STUDY WE WILL IN ADDITION USE TILES AS SMALL AS 5 DEGREES FOR A BETTER SPATIAL AND TEMPORAL RESOLUTION NEAR THE SURFACE AND BIG TILES OF 30 DEGREE TO COVER THE NSSL. WE WILL THEN CUSTOMIZE THE RING-DIAGRAM ANALYSIS MODIFYING THE GRID SIZE AS WELL AS THE GRID SPACING AND THE TRACKING RATE TO OPTIMIZE THE ANALYSIS FOR THE PROPOSED PROJECT. WE WILL DERIVE THE SYSTEMATIC VARIATIONS OF THE FLOWS WITH DISK POSITION AND CORRECT THEM. TO DERIVE THE FLOWS NEAR THE NSSL WE WILL ALSO APPLY HELIOSEISMIC TIME-DISTANCE ANALYSIS TO SDO/HMI DOPPLERGRAMS. SINCE TIMEDISTANCE AND RING-DIAGRAM ANALYSES HAVE DIFFERENT ERROR CHARACTERISTICS THIS WILL ALLOW US TO CROSS-VALIDATE THE RESULTS FROM BOTH TECHNIQUES. TO DERIVE FLOWS AT THE SOLAR SURFACE WE WILL USE F-MODES DERIVED FROM SDO/HMI DOPPLERGRAMS AND AN APPROPRIATE LCT TECHNIQUE APPLIED TO SDO/HMI DOPPLERGRAMS AND VECTOR MAGNETOGRAMS. THIS WILL ALLOW US TO COMPARE THREE SETS OF SURFACE FLOWS FROM DIFFERENT TECHNIQUES AND DATA SETS. PROPOSED CONTRIBUTIONS TO THE FOCUS TEAM EFFORT: THE PROPOSED STUDY OF THE LARGE-SCALE FLOWS IN THE UPPER CONVECTION ZONE WILL PROVIDE OBSERVATIONAL CONSTRAINTS WHICH WILL BE CRUCIAL FOR THE MODELING OF THE SOLAR INTERIOR AND THE SOLAR FLUX TRANSPORT. THIS WILL LEAD TO A BETTER UNDERSTANDING OF THE GENERATION AND EVOLUTION OF GLOBAL-SCALE MAGNETIC FIELDS AND AS A CONSEQUENCE PROVIDE CONSTRAINTS FOR FORECASTING SOLAR ACTIVITY. THE PROPOSED STUDY THEREFORE ADDRESSES THE OBJECTIVE OF FOCUSED SCIENCE TOPIC (4): UNDERSTANDING GLOBAL-SCALE SOLAR PROCESSES AND THEIR IMPLICATIONS FOR THE SOLAR INTERIOR.

FORMATION & EVOLUTION OF MASSIVE STELLAR SPHEROIDS FROM RECOMBINATION TO THE PRESENT FOR THE NEXT

THE WAYS IN WHICH GALAXIES ACQUIRE PROCESS ENRICH AND EXPEL THEIR GAS---KNOWN AS THE "BARYON CYCLE"---ARE AMONG THE MOST COMPLEX AND IMPORTANT PROCESSES IN ASTROPHYSICS. HUBBLE AND ITS CONTEMPORARIES HAVE REVEALED MUCH ABOUT THE GAS-GALAXY CONNECTION AT Z<1. WE ANTICIPATE RAPID PROGRESS IN OBSERVATIONAL STUDIES OF THE GAS-GALAXY CONNECTION AT THE Z>2 EPOCH THANKS TO JWST WHICH WILL REACH MUCH DEEPER INTO THE GALAXY POPULATION AND TO MUCH HIGHER REDSHIFTS THAN HAS BEEN POSSIBLE TO DATE DRAWING A RICHER PICTURE OF THIS CONNECTION WHEN ADDED TO THE ALREADY LARGE BODY OF GROUND-BASED SPECTROSCOPY OF THE GAS. TO ADDRESS THE BARYON CYCLE AT Z<1 OUR GROUP HAS DEVELOPED NOVEL APPROACHES TO SIMULATING THE GAS-GALAXY CONNECTION AND SYNTHESIZING MOCK DATA. WE HAVE ACHIEVED 10^4-5 TIMES FINER MASS RESOLUTION IN GALACTIC GAS FLOWS THAN CONVENTIONAL COSMOLOGICAL SIMULATIONS AND WE ARE DEVELOPING NEW TOOLS FOR MAKING SYNTHETIC DATA. WE PROPOSE TO APPLY THESE NEW TECHNIQUES AT Z>2 WHEN STAR FORMATION AND BLACK HOLE ACCRETION RATES WERE RISING WHEN THE POTENTIAL IMPACTS FOR FEEDBACK ON THE BARYON CYCLE ARE STRONGEST. NEW DATA EXPECTED FROM JWST WILL REVOLUTIONIZE THE GALAXY SIDE OF THE GAS/GALAXY EQUATION AT THESE REDSHIFTS OFFERING A NEW WINDOW INTO THE IMPORTANT PHYSICS AND DRAWING SOLID LINKS TO HUBBLE'S WORK AT Z<1. FULLY INTERPRETING THESE NEW DATA HOWEVER WILL REQUIRE NEW THEORETICAL MODELS SYNTHETIC OBSERVATIONS AND ANALYSIS METHODS: FOGGIE WILL EXPLORE BOTH THE PHYSICAL AND OBSERVABLE EFFECTS OF FEEDBACK ON Z>2 GALAXIES. OUR MAIN SCIENTIFIC GOAL FOR THIS WORK IS TO UNDERSTAND THE CGM AND ISM GAS PROCESSES THAT GOVERN STAR FORMATION AND MORPHOLOGY IN OBSERVABLE WAYS. WE WILL FOCUS ON FOUR INTER-RELATED SCIENCE QUESTIONS: (1) STARS: HOW DO FEEDBACK ACCRETION AND GAS RECYCLING AFFECT RESOLVED STAR FORMATION HISTORIES? (2) ISM: HOW DO STAR FORMATION AND AGN FEEDBACK AFFECT THE PHYSICAL PROPERTIES OF THE ISM AT Z>2 AND WHAT DIAGNOSTICS ACCURATELY TRACE THESE PROPERTIES? (3) CGM: HOW DOES FEEDBACK AFFECT THE PHYSICAL AND OBSERVABLE PROPERTIES OF THE CGM? (4) METALS: HOW DOES FEEDBACK AFFECT GALACTIC METAL BUDGETS AND METALLICITY SCALING RELATIONS? WE WILL ADDRESS THESE IMPORTANT QUESTIONS WITH A NOVEL COMBINATION OF EXTREME RESOLUTION IN THE GAS FLOWS AROUND GALAXIES A SUITE OF SYNTHETIC DATA AND NEW TREATMENTS OF STELLAR AND AGN FEEDBACK. WE PLAN TO ADDRESS THESE UNANSWERED QUESTIONS WITH A MAJOR STEP FORWARD IN OUR ABILITY TO ANALYZE THE CONNECTION BETWEEN GALAXIES AND THEIR CIRCUMGALACTIC GAS. OUR PROGRAM CONSISTS OF (1) A NEW SUITE OF COSMOLOGICAL HYDRODYNAMIC SIMULATIONS OF UNPRECEDENTED RESOLUTION IN THE GAS FLOWS AROUND AND WITHIN GALAXIES (2) A NOVEL REFINEMENT SCHEME FOR ACHIEVING THIS RESOLUTION (3) SYNTHETIC OBSERVATIONS OF SIMULATION DATA AND AN OPEN-SOURCE PIPELINE FOR PRODUCING MOCK DATA FROM OTHER SIMULATIONS AND (4) A NOVEL APPROACH TO VARYING FEEDBACK RECIPES AND ASSESSING THEIR EFFECTS ON OBSERVABLE DATA OF BOTH STARS AND GAS. OUR GOALS ARE CONSISTENT WITH NASA'S STRATEGIC OBJECTIVE 1.6 TO "DISCOVER HOW THE UNIVERSE WORKS. . . ". WE WILL PROVIDE PHYSICAL MODELS AND SYNTHETIC DATA FOR COMPARISONS TO OBSERVATIONS FROM CURRENT AND FUTURE NASA FACILITIES SUCH AS HUBBLE AND JWST. WITH JWST SET TO BE COMMISSIONED FOR SCIENCE BY SPRING 2019 (BEFORE THE NEXT ATP DEADLINE) IT IS IMPORTANT THAT WE BEGIN THIS WORK NOW.

LA SERENA SCHOOL FOR DATA SCIENCE: APPLIED TOOLS FOR ASTROINFORMATICS, BIOMEDICAL INFORMATICS, AND OTHER DATA-DRIVEN SCIENCES

THE PRIMARY GOALS OF THIS PROPOSAL ARE TO PRODUCE CHARACTERIZE AND DETERMINE OPTICAL PROPERTIES OF STARDUST ANALOGS COMPOSED OF ALUMINUM AND OXYGEN

DATA DRIVEN INVESTIGATIONS OF CGI AS A STARLIGHT SUPPRESSION YARDSTICK.

NON-REDUNDANT MASKING (NRM) IS A HIGH CONTRAST, HIGH RESOLUTION TECHNIQUE RELEVANT TO FUTURE SPACE MISSIONS CONCERNED WITH EXTRA SOLAR PLANETARY SYST

SCIENCE GOALS AND OBJECTIVES: THE MERIDIONAL FLOW PLAYS AN IMPORTANT ROLE IN THE UNDERSTANDING OF A BROAD RANGE OF SOLAR PHENOMENA. FOR EXAMPLE THE SPEED AND PROFILE OF THE MERIDIONAL FLOW DETERMINES THE DURATION OF THE SOLAR CYCLE IN FLUX-TRANSPORT DYNAMO MODELS ITS RISE AND FALL PATTERN THE POLAR FIELD STRENGTH AND THE TIMING OF ITS REVERSAL. THE STRENGTH OF THE POLAR FIELD OF THE PREVIOUS MINIMUM PLAYS AN IMPORTANT ROLE IN DETERMINING THE STRENGTH OF THE NEXT CYCLE. THEREFORE IT IS IMPORTANT TO KNOW THE EVOLUTION OF THE POLAR FIELD WHICH IS LARGELY GOVERNED BY THE TRANSPORT BY MERIDIONAL CIRCULATION. WE PROPOSE TO STUDY THE MERIDIONAL FLOW IN THE SOLAR CONVECTION ZONE FROM THE SURFACE TO THE NEAR-SURFACE SHEAR LAYER USING RING-DIAGRAM ANALYSIS AND IN THE LOWER CONVECTION ZONE USING TIME-DISTANCE ANALYSIS ANALYZING SDO/HMI DOPPLERGRAMS. WE WILL THEN ASSIMILATE THE MERIDIONAL FLOW AND THE SURFACE MAGNETIC FIELD FROM SDO/ HMI INTO FLUX-TRANSPORT DYNAMO MODELS AND DRIVE THE MODELS WITH THE FLOWS. TO COVER MORE THAN ONE SOLAR CYCLE WE WILL ANALYZE MDI DATA SETS. THE GOALS OF THE PROPOSED PROJECT ARE (I) TO DETERMINE THE INFLUENCE OF THE MERIDIONAL FLOW ON DYNAMO-GENERATED MAGNETIC FIELDS DURING DIFFERENT PHASES OF THE SOLAR CYCLE AND (II) TO USE THE RESULTS TO PREDICT THE POLAR FIELDS DURING THE UPCOMING CYCLE MINIMUM AND THE STRENGTH OF CYCLE 25. THIS IS TIMELY SINCE SDO/HMI OBSERVATIONS COVER SOLAR CYCLE 24 AND THE HIGH SPATIAL RESOLUTION OF HMI ALLOWS US TO MEASURE SUBSURFACE MERIDIONAL FLOWS AT HIGH LATITUDES TO ABOUT 75 DEGREE. BY ASSIMILATING MERIDIONAL FLOWS AND SURFACE MAGNETIC FIELDS FROM SDO/HMI INTO DYNAMO MODELS WE WILL BE ABLE TO DETERMINE HOW WELL FLOW MEASUREMENTS CAN CONSTRAIN THE DYNAMO. RELEVANCE: THIS PROPOSAL DIRECTLY ADDRESSES THE FIRST SCIENCE GOAL FROM THE HELIOPHYSICS DECADAL SURVEY: DETERMINE THE ORIGINS OF THE SUN S ACTIVITY AND PREDICT THE VARIATIONS IN THE SPACE ENVIRONMENT . THE WORK PROPOSED HERE WILL GREATLY ENHANCE THE SCIENTIFIC RETURN OF THE SDO/HMI MISSION. METHODOLOGY: WE PROPOSE TO DETERMINE THE MERIDIONAL FLOW FROM SDO/HMI DOPPLERGRAMS USING TWO DIFFERENT HELIOSEISMIC TECHNIQUES. TO DETERMINE THE MERIDIONAL FLOW FROM THE SURFACE TO A DEPTH OF ABOUT 40 MM ON TIME SCALES OF DAYS AND MONTHS WE WILL USE RINGDIAGRAM ANALYSIS WITH THREE TILE SIZES. TO DISCERN THE CONTRIBUTIONS FROM ACTIVE REGIONS WE WILL STUDY FLOWS FROM SMALL 5 DEGREE TILES. TO REACH DEPTHS OF ABOUT 40 MM AND STUDY THE INFLUENCE OF THE NEAR-SURFACE SHEAR LAYER WE WILL USE FLOWS FROM 30 DEGREE TILES. WE WILL CROSS-VALIDATE THESE RESULTS WITH THOSE FROM THE STANDARD 15 DEGREE TILES COVERING DEPTHS FROM THE SURFACE TO ABOUT 16 MM. TO DETERMINE THE MERIDIONAL FLOW IN THE LOWER HALF OF THE CONVECTION ZONE ON TIME SCALES OF TWO YEARS WE WILL USE A CUSTOMIZED TIMEDISTANCE ANALYSIS. THE KEY POINT IS TO PERFORM THE ANALYSIS IN SPHERICAL GEOMETRY WHICH ALLOWS US TO ISOLATE ACOUSTIC WAVES PROPAGATING TO DEEP LAYERS. THIS WILL ALLOW US TO CONSTRAIN THE RETURN FLOW NEAR THE BASE OF THE CONVECTION ZONE AND THE NUMBER OF CELLS WITH DEPTH. WE WILL USE AN ENSEMBLE KALMAN FILTER TO ASSIMILATE THE SUBSURFACE MERIDIONAL FLOW AND THE SURFACE MAGNETOGRAMS INTO THE DYNAMO MODEL AND OPERATE THE MODEL IN THE ANALYSES AND THE FORECAST MODE SO THAT WE CAN RESOLVE UNCERTAINTIES IN MODEL INGREDIENTS IN THE ANALYSES PHASE AND CORRECTLY HINDCAST AND FORECAST THE POLAR FIELDS AND PROPERTIES OF SOLAR CYCLES 24 AND 25 IN THE FORECAST PHASE. WE WILL CHECK THE CONSISTENCY BETWEEN THE MERIDIONAL FLOWS DETERMINED IN THE UPPER AND LOWER CONVECTION ZONE ON DIFFERENT TEMPORAL AND SPATIAL SCALES AS WELL AS WHETHER THE MODEL WORKS BEST WITH HIGH OR LOW MAGNETIC DIFFUSIVITY. WE WILL DETERMINE THE CONSEQUENCES OF THE MERIDIONAL FLOW AT HIGH LATITUDES FOR THE POLEWARD FLUX TRANSPORT AND POLAR FIELD FEATURES AND IN TURN FOR THE CYCLE 25 AMPLITUDE

ENHANCING THE ROMAN COSMOLOGY PROGRAM WITH STRONGLY LENSED SUPERNOVAE

LOOKING AT THE DIFFUSE GALACTIC ISM FROM BELOW IN RADIO OR INFRARED EMISSION WE SEE A CACOPHONY OF MAGNIFICENT STRUCTURES. THE CLOUDS OF NEUTRAL GAS THAT STRETCH ACROSS THE HIGH-LATITUDE SKY VARY IN TEMPERATURE VELOCITY MORPHOLOGY AND

WE DESCRIBE A FOUR YEAR PLAN TO CONTINUE DISCOVERING AND CHARACTERIZING PLANETS THAT TRANSIT BRIGHT STARS. TO DATE ASTRONOMERS HAVE REPORTED MORE THAN 30 SUCH TRANSITING PLANETS ORBITING BRIGHT STARS AND THEIR NUMBERS ARE INCREASING RAPIDLY (BOTH THE NUMBER OF PLANETS AND THE NUMBER OF ASTRONOMERS STUDYING THEM). THE BRIGHTEST TYPICALLY ARE DISCOVERED BY OSCILLATING RADIAL VELOCITIES AND SOMEWHAT FAINTER ONES IN MUCH LARGER NUMBERS ARE DISCOVERED BY TRANSITS. THE XO OBSERVATORY HAS RECENTLY BEEN EXPANDED TO SIX 0.1-METER DIAMETER CAMERAS TWO OF WHICH HAVE BEEN OPERATING ROBOTICALLY SINCE SEP 2003 AND WITH WHICH WE HAVE DISCOVERED FIVE TRANSITING PLANETS. BY DEC 31 2013 XO WILL HAVE OBSERVED 90% OF THE NORTHERN SKY WITH TWO LENSES FOR TWO SEASONS PERMITTING ITS TEAM AND OTHERS TO DISCOVER AND CHARACTERIZE TRANSITING EXTRASOLAR PLANETS (TEPS). WE EVALUATE TRANSITING-PLANET CANDIDATES PRODUCED BY THE XO SURVEY CAMERAS WITH PRECISE PHOTOMETRIC OBSERVATIONS WHICH SIGNIFICANTLY REDUCES THE NUMBER OF CANDIDATES WE OBSERVE SPECTROSCOPICALLY. FOR THE FOLLOW-UP PHOTOMETRY WE HAVE RECRUITED A GLOBAL NETWORK OF AMATEUR ASTRONOMERS IN ADDITION TO OUR TEAM'S INSTITUTIONAL ACCESS TO OBSERVATORIES IN TEXAS AND ARIZONA. DOZENS OF CANDIDATES PER YEAR WILL BE SCRUTINIZED WITH MODERATE-PRECISION (1 KM/S) RADIAL VELOCITY OBSERVATIONS AND A FEW OF THOSE WILL BE CONFIRMED TO BE PLANETS WITH (5 M/S) PRECISION. WE WILL PURSUE PRECISE PHOTOMETRIC AND SPECTROSCOPIC FOLLOW UP OBSERVATIONS OF TRANSITING PLANETS. OUR TEAM HAS PRIOR EXPERIENCE WITH SCINTILLATION-LIMITED GROUND-BASED PHOTOMETRY TIME-SERIES PHOTOMETRY WITH SST IRAC SPECTROPHOTOMETRY WITH HST INSTRUMENTS NICMOS STIS FGS ACS AND WFC3 (IN GROUND-TESTS) AND IS DEVELOPING SPECTROSCOPIC ANALYSIS TECHNIQUES TO IMPROVE THE PRECISION OF RADIAL VELOCITIES FROM THE HET AND KECK. USING RADIAL VELOCITIES AND PHOTOMETRY WE WILL SEARCH FOR ADDITIONAL COMPANIONS AROUND STARS KNOWN TO HOST A TRANSITING PLANET. FOR THE PERIOD 2003-2009 THE XO TEAM HAS BEEN SUPPORTED BY TWO NASA ORIGINS AWARDS. FOLLOW-UP OBSERVATIONS WITH HST AND SST HAVE BEEN SUPPORTED BY THOSE NASA PROGRAMS. THE TRIPLING OF XO'S CAMERAS AND ASSOCIATED ELECTRONICS HAS BEEN SUPPORTED BY PEER-REVIEWED COMPETITION FOR INSTITUTIONAL FUNDS OF THE STSCI DIRECTOR.

PROJECT SUMMARY IN THIS PROPOSAL, I OUTLINE MY PLANS TO PREPARE MY GUARANTEED TIME OBSERVATIONS (GTO) PROGRAM FOR THE JAMES WEBB SPACE TELESCOPE (JWS

THIS PROPOSAL TARGETS THE INSTRUMENT AND TECHNOLOGY DEVELOPMENT (ITD) ELEMENT OF THE H-TIDES PROGRAM. MAGNETIC FIELDS FORM A FOUNDATION FOR ALL SOLAR ACTIVE PHENOMENA FROM TINY G-BAND BRIGHT POINTS TO SUNSPOTS AND CORONAL MASS EJECTIONS (CMES). THEY SERVE AS A RESERVOIR OF ENERGY FOR FLARES PLAY A CRITICAL ROLE IN TRIGGERING MECHANISMS FOR CMES AND PROVIDE THE MEANS OF TRANSPORTING ENERGY FROM THE PHOTOSPHERE TO CORONA. THUS ARGUABLY THE MAGNETOGRAPH SHOULD BE CONSIDERED AS A CRITICAL INSTRUMENT FOR EVERY HELIOPHYSICS MISSION THAT STUDIES THE SOLAR ATMOSPHERE OR THE EFFECTS OF SOLAR ACTIVITY ON HELIOSPHERE. WHILE THE IMPORTANCE OF MAGNETOGRAPH INSTRUMENT IS WIDELY RECOGNIZED BY THE COMMUNITY IN PRACTICE THEIR INCLUSION AS A SPACECRAFT PAYLOAD IS OFTEN LIMITED DUE TO WEIGHT AND SIZE RESTRICTIONS. THE MAGNETOGRAPH CONCEPTS WHICH ARE CURRENTLY IN USE REQUIRE SAMPLING A MAGNETO-SENSITIVE SPECTRAL LINE AT DIFFERENT POSITIONS ACROSS SOLAR DISK. SPECTROGRAPH-BASED MAGNETOGRAPHS ARE SUPERIOR IN TERMS OF SPECTRAL SAMPLING BUT REQUIRE SCANNING OF SOLAR IMAGE TO BUILD UP ITS MAGNETIC MAP. NARROW-BAND FILTER-BASED MAGNETOGRAPHS TAKE SIMULTANEOUS SNAPSHOTS OF EXTENDED AREA OF SOLAR SURFACE BUT REQUIRE TAKING MULTIPLE OBSERVATIONS WITH DIFFERENT WAVELENGTH OFFSET BETWEEN SEPARATE FRAMES. BOTH APPROACHES MAY REQUIRE RELATIVELY LARGE NUMBER OF OPTICAL AND ELECTRO-MECHANICAL ELEMENTS FOR SPECTRAL TUNING AND/OR SPATIAL SCANNING. THESE ADDITION ELEMENTS TEND TO INCREASE THE OVERALL WEIGHT AND SIZE OF INSTRUMENT AND THE ADDED COMPLEXITY MIGHT AFFECT THE RELIABILITY OF SYSTEM. GOALS AND OBJECTIVES: AS THE MAIN GOAL OF THIS PROJECT WE WILL EXPLORE A NOVEL ALTERNATIVE TO THE STANDARD FILTER BASED MAGNETOGRAPH WHICH WE CALL THE SIMPLEST MAGNETOGRAPH. THE PROPOSED INSTRUMENT CONCEPT IS BASED ON MEASURING A BROAD-BAND POLARIZATION OVER THE WHOLE LINE PROFILE WHICH COULD BE DONE WITHOUT MOVING OPTICAL ELEMENTS AND COMPLICATED OPTICAL SCHEMES. IF SUCCESSFUL THIS CONCEPT WILL LEAD TO CREATION OF EXTREMELY SIMPLE AND COMPACT LINE-OF-SIGHT (LOS) OR FULL VECTOR MAGNETOGRAPH SUITABLE FOR SPACE MISSIONS. SUCH INSTRUMENT COULD BE ESPECIALLY ATTRACTIVE FOR SPACE WEATHER-ORIENTED MISSIONS. THE METHODOLOGY: THE CONCEPT OF THE PROPOSED MAGNETOGRAPH IS BASED ON A WELL-KNOWN FACT THAT ZEEMAN SPLIT SPECTRUM LINES IN A LINEOF- SIGHT (LOS) FIELD ARE ASYMMETRIC WITH ONE OF THE V STOKES PROFILE LOBES STRONGER THAN THE OTHER IN A WAY THAT SWITCHES WITH POLARITY. IN TRANSVERSE FIELD THERE IS A NET LINEAR POLARIZATION AVERAGED ACROSS THE LINE PROFILE BECAUSE THE CENTRAL PART OF THE SPECTRUM LINE IS SATURATED RELATIVE TO THE WINGS SO THE WING POLARIZATION DOMINATES IN Q AND U POLARIZATION PROFILES. THUS MEASURING NET POLARIZATION OVER THE ENTIRE SPECTRAL LINE PROFILE (WITHOUT SCANNING IN SPECTRAL OR SPATIAL DIRECTIONS) ALLOWS TO DETERMINE BOTH POLARITY AND THE FIELD STRENGTH (MAGNETIC FLUX) FOR EACH PIXEL OF IMAGE. PRELIMINARY TESTS WITH STOKES-V SPECTRA TAKEN WITH GONG INSTRUMENT SUPPORT THE FEASIBILITY OF THIS APPROACH. PROPOSED CONTRIBUTION: THE NSO TEAM WILL INVESTIGATE THE CONCEPT OF THIS SIMPLEST MAGNETOGRAPH BOTH VIA MODELING AND LABORATORY MEASUREMENTS. WE WILL ALSO BUILD A PROTOTYPE INSTRUMENT. THE PERFORMANCE OF THIS MAGNETOGRAPH WILL BE TESTED AT THE GROUNDBASED TELESCOPES OPERATED BY THE NSO. IN ADDITION THE PROTOTYPE INSTRUMENT CAN BE PROPOSED FOR FLIGHT ON THE INTERNATIONAL SPACE STATION AND PERHAPS ALSO ON MISSION OF OPPORTUNITIES SUCH AS THE UK/EU LAGRANGE L5 MISSION.

PRECISION CLUSTER COSMOLOGY WITH INTERPRETABLE MACHINE LEARNING

CAPITALIZING ON A RECENT BREAKTHROUGH IN WAVEFRONT CONTROL THEORY FOR OBSCURED APERTURES MADE BY OUR GROUP, WE PROPOSE TO DEMONSTRATE A METHOD TO ACH

IN 1609 GALILEO GALILEI TURNED A NEW PIECE OF TECHNOLOGY TOWARDS THE HEAVENS TRIGGERING A SCIENTIF

WE PROPOSE AN ADAP PROGRAM TO CONDUCT A COMPREHENSIVE UV SPECTROSCOPIC ANALYSIS OF ALL 18 ARCHIVAL FUSE AND IUE SPECTRA OF MASSIVE STARS IN THE GC REGION.

SCIENCE GOALS AND OBJECTIVES: WE PROPOSE TO PERFORM A COMPREHENSIVE STUDY OF THE SUBSURFACE AND SURFACE FLOWS ASSOCIATED WITH ACTIVE REGIONS AND THEIR EVOLUTION USING SDO/HMI DOPPLERGRAMS AND MAGNETOGRAMS. THE EVOLUTION OF ACTIVE REGIONS IS OF FUNDAMENTAL IMPORTANCE IN SOLAR PHYSICS. SINCE ACTIVE REGIONS ARE FORMED FROM STRONG MAGNETIC FIELDS GENERATED BY A SOLAR DYNAMO LOCATED IN THE SOLAR INTERIOR THEIR EVOLUTION FROM EMERGENCE THROUGH DECAY PROVIDES CRUCIAL INFORMATION ABOUT THE SOLAR DYNAMO AND THUS ABOUT THE ORIGINS OF THE SUN S ACTIVITY. SUBSURFACE FLOW PARAMETERS CAN SERVE AS PROXIES OF THE MAGNETIC STRUCTURE IN SUBSURFACE LAYERS AND LINK THE DYNAMICS OF SUBSURFACE LAYERS WITH THE CONDITIONS OF THE MAGNETIC ACTIVITY IN THE PHOTOSPHERE AND ABOVE. STUDIES OF SUBSURFACE FLOWS HAVE FOCUSED MAINLY ON FLARE-PRODUCTIVE REGIONS OR ON THE EMERGENCE OF ACTIVE REGIONS. HOWEVER A SYSTEMATIC STUDY OF THE EVOLUTION OF SUBSURFACE FLOWS OF ACTIVE REGIONS FROM EMERGENCE TO DECAY WITH REGARD TO THEIR MORPHOLOGY HAS YET TO BE PERFORMED. ACTIVE REGIONS EVOLVE DURING THEIR LIFE TIME AND THE SUBSURFACE FLOWS ARE EXPECTED TO CHANGE AS WELL. WE PROPOSE TO STUDY THE SUBSURFACE FLOWS OF ACTIVE REGIONS OBSERVED BY SDO/HMI THROUGHOUT THE SOLAR CYCLE. WE WILL FOCUS ON FOR EXAMPLE LONG-LIVED ACTIVE REGIONS EMERGING AND DECAYING REGIONS FLARING AND NON-FLARING REGIONS AND REGIONS WITH AND WITHOUT ROTATING SUNSPOTS. THE GOAL IS TO ESTABLISH COMMON FEATURES OF THE SUBSURFACE DYNAMICS OF ACTIVE REGIONS AND DIFFERENTIATE THEM FROM CHARACTERISTICS THAT DEPEND ON THEIR MORPHOLOGY. THE RESULTING FLOW PROFILES WILL PROVIDE CRUCIAL INFORMATION ABOUT THE MAGNETIC FLUX OF ACTIVE REGIONS AND HOW IT IS SYNTHESIZED CONCENTRATED AND DISPERSED.DATA: WE WILL USE DOPPLERGRAMS AND MAGNETOGRAMS OBTAINED BY THE HMI INSTRUMENT ONBOARD THE SDO SPACECRAFT. THESE HIGHRESOLUTION OBSERVATIONS ALLOW US TO MEASURE SUBSURFACE FLOWS AT GREAT DISTANCES FROM DISK CENTER AND THUS FOLLOW THE EVOLUTION OF ACTIVE REGIONS DURING THEIR DISK PASSAGE FOR A MUCH LONGER PERIOD OF TIME THAN POSSIBLE WITH PREVIOUS OBSERVATIONS. THE AVAILABILITY OF SIMULTANEOUS VECTOR MAGNETOGRAMS WILL ALLOW US TO FOLLOW THE EVOLUTION OF ACTIVE REGIONS AT THE SOLAR SURFACE AND TO DERIVE SURFACE FLOWS AS WELL. METHODOLOGY: WE WILL PERFORM A COMPREHENSIVE STUDY OF THE SUBSURFACE AND SURFACE FLOWS OF ACTIVE REGIONS AND THEIR TEMPORAL AND SPATIAL EVOLUTION. WE WILL DERIVE THE SUBSURFACE FLOWS DURING THE DISK PASSAGE OF EACH ACTIVE REGION WITH RING-DIAGRAM AND TIMEDISTANCE ANALYSIS (TWO WELL-ESTABLISHED HELIOSEISMIC TECHNIQUES) OF HMI DOPPLERGRAMS. IN ADDITION TO USING FLOWS FROM THE HMI RING-DIAGRAM PIPELINE WE WILL CUSTOMIZE THE TECHNIQUES TO DERIVE FLOWS ON A FINER TEMPORAL AND SPATIAL GRID APPROPRIATE FOR ACTIVE REGIONS. AT THE SURFACE FLOWS AND EVOLUTION OF MAGNETIC ACTIVITY WILL BE DERIVED FROM THE CORRESPONDING HMI VECTOR MAGNETOGRAMS USING ESTABLISHED CORRELATION TRACKING TECHNIQUES TO DERIVE SURFACE FLOWS. THIS WILL ALLOW US TO MATCH THE SURFACE WITH THE SUBSURFACE EVOLUTION OF ACTIVE REGIONS. RELEVANCE: THE PROPOSED STUDY OF SUBSURFACE DYNAMICS OF ACTIVE REGIONS WILL LEAD TO A BETTER UNDERSTANDING OF THE EVOLUTION OF ACTIVE REGIONS. THE PROPOSAL IS THUS RELEVANT TO THE FOLLOWING GOAL OF THE SDO PROJECT: HOW IS ACTIVE REGION MAGNETIC FLUX SYNTHESIZED CONCENTRATED AND DISPERSED ACROSS THE SOLAR SURFACE? THE PROPOSAL ALSO ADDRESSES THE GOAL DETERMINE THE ORIGINS OF THE SUN S ACTIVITY AND PREDICT THE VARIATIONS IN THE SPACE ENVIRONMENT FROM THE HELIOPHYSICS DECADAL SURVEY.

THE PROPOSED EFFORT WILL DETERMINE THE CONTRIBUTION OF SUBSURFACE FLOWS OF ACTIVE REGIONS (ESPECIALLY INFLOWS AND OUTFLOWS) ON FLUX CANCELLATION AT LOW LATITUDES AND THUS ON THE RESULTING POLEWARD MIGRATION OF MAGNETIC ACTIVITY OF OPPOSITE POLARITY. THIS WILL BE CARRIED OUT THROUGH A STATISTICAL STUDY OF THE SUBSURFACE FLOWS NEAR ACTIVE REGIONS AND THE CORRESPONDING MAGNETIC FLUX DURING SOLAR CYCLES 24 AND 25. THE STUDY WILL INVESTIGATE IF SUCH FLOWS SHOULD BE INCLUDED AS KEY INGREDIENTS IN SURFACE FLUX TRANSPORT MODELS AND AS A CONSEQUENCE IN SOLAR CYCLE PREDICTIONS. THE GOAL IS TO DERIVE THE ROLE OF THESE SUBSURFACE FLOWS IN MAGNETIC FLUX TRANSPORT. SURFACE FLUX TRANSPORT MODELS ALREADY INCLUDE INFORMATION ABOUT POLEWARD MERIDIONAL FLOW AND DIFFUSION TO MODEL THE EVOLUTION OF THE MAGNETIC FIELD AND ACTIVITY CYCLE. SOME OF THESE MODELS EXPLAIN THE AMPLITUDE VARIABILITY OF THE SOLAR CYCLE WITH INFLOWS TOWARD ACTIVE REGIONS AND RARE EVENTS SUCH AS CROSS-EQUATORIAL FLUX PLUMES. CROSS-EQUATORIAL MERIDIONAL FLOW IS ONE OF THE PROCESSES THAT MAY LEAD TO MAGNETIC FLUX CANCELLATION LATE IN THE SOLAR CYCLE WHERE FIELDS WITH OPPOSITE POLARITY COME IN CLOSE PROXIMITY AND CANCEL EACH OTHER ACROSS THE EQUATOR. SIMULATIONS HAVE SHOWN THAT EVEN SINGLE BIG ACTIVE REGIONS NOT FOLLOWING JOY'S LAW EMERGING VERY NEAR OR ACROSS THE SOLAR EQUATOR CAN SIGNIFICANTLY AFFECT THE AMPLITUDE OF THE POLAR FIELD. WHILE SUBSURFACE FLOWS OF ACTIVE REGIONS AND LARGE-SCALE FLOWS HAVE BEEN STUDIED BEFORE THEIR SPECIFIC ROLE IN MAGNETIC FLUX TRANSPORT HAVE NOT YET BEEN EXPLORED. PROPOSED STUDY WILL LEAD TO A BETTER UNDERSTANDING OF THE INTERCONNECTION BETWEEN SUBSURFACE FLOW PATTERNS NEAR ACTIVE REGIONS AND SURFACE FLUX TRANSPORT. THE PROPOSAL IS THUS RELEVANT TO THE FOLLOWING GOAL OF THE SDO PROJECT: HOW IS ACTIVE REGION MAGNETIC FLUX SYNTHESIZED CONCENTRATED AND DISPERSED ACROSS THE SOLAR SURFACE? THE PROPOSAL ALSO ADDRESSES THE GOAL DETERMINE THE ORIGINS OF THE SUN'S ACTIVITY AND PREDICT THE VARIATIONS IN THE SPACE ENVIRONMENT FROM THE HELIOPHYSICS DECADAL SURVEY.

THE CITIZEN CONTINENTAL-AMERICA TELESCOPIC ECLIPSE (CATE) EXPERIMENT IS BEING DEVELOPED AT THE NATIONAL SOLAR OBSERVATORY IN PARTNERSHIP WITH UNIVERS

WE OBSERVED THE ENTIRE SMALL MAGELLANIC CLOUD INCLUDING THE BAR WING AND BRIDGE WITH THE SPITZER SPACE TELESCOPE IN TWO EPOCHS THREE MONTHS APART IN CYCLE 13. THESE OBSERVATIONS REPEAT THE FOOTPRINT OBTAINED FROM THE SAGE-SMC PROGRAM (SURVEYING THE AGENTS OF GALACTIC EVOLUTION) IN 2008 GIVING US A MINIMUM OF FOUR EPOCHS COVERING THE ENTIRE GALAXY WITH A TEMPORAL BASELINE OF NEARLY A DECADE. THESE DATA WILL FACILITATE THE CHARACTERIZATION OF THE POPULATION OF VARIABLE STARS IN THE SMC (ESPECIALLY DUSTY AND LONG-PERIOD VARIABLES) THE SEARCH FOR INFRARED TRANSIENTS IN THAT PART OF THE SKY AND THE SEARCH FOR GALACTIC BROWN DWARFS IN THE FOREGROUND. THE KEY TO ENABLING THIS SCIENCE IS TO PRODUCE CATALOGS WITH GOOD ASTROMETRIC AND PHOTOMETRIC FIDELITY. WE ARE THUS PROPOSING AN ASTROPHYSICAL DATABASE PROJECT FOR THIS PURPOSE. WITH SUPPORT FROM NASA'S ASTROPHYSICS DATA ANALYSIS PROGRAM WE WILL GENERATE MOSAICS AND EXTRACT ALL POINT SOURCES FROM THE NEW DATA AND ENSURE THAT THEY CONFORM TO EXTRACTIONS OF THE TWO SHORT-WAVELENGTH FILTERS ON THE INFRARED ARRAY CAMERA FROM THE SAGE-SMC PROGRAM AS WELL AS OTHER PROGRAMS THAT PROVIDED FIVE ADDITIONAL EPOCHS IN THE CORE OF THE SMC IN 2005 AND 2010-2011. WE WILL SUPPLY THE MOSAICS AND CATALOGS TO THE COMMUNITY VIA THE INFRARED SCIENCE ARCHIVE (IRSA) WHERE THEY WILL BE AVAILABLE FOR A MULTITUDE OF SCIENCE PROJECTS WELL BEYOND THOSE DESCRIBED HERE.

THE PROPOSED WORK WILL PROVIDE A UNIQUE STUDY OF THE DYNAMICS OF NSSL USING THE LONGEST DATA SET PROCESSED IN A SELF-CONSISTENT MANNER.

SUPPORT FOR CO-I CONTRIBUTIONS TO THE KEPLER MISSION: 1. DESCRIBE UNIQUE INNOVAT

ENABLING FUTURE EXO-EARTH IMAGING SPACE TELESCOPES SUCH AS THE HABEX AND LUVOIR MISSION CONCEPTS REQUIRES FURTHER ADVANCES IN THE STATE OF THE ART OF WAVEFRONT SENSING AND CONTROL (WFS&C) METHODS PARTICULARLY METHODS FOR CONTINUOUSLY MAINTAINING U

EXECUTE A BALANCED SCIENCE PROGRAM BASED ON DISCIPLINE-SPECIFIC GUIDANCE FROM THE NATIONAL ACADEMIES OF SCIENCES ENGINEERING AND MEDICINE ADMINISTRATION PRIORITIES AND DIRECTION FROM CONGRESS. PARTICIPATE AS A KEY PARTNER AND ENABLER IN THE AGENC

GALAXIES LIE AT THE CONFLUENCE OF LARGE-SCALE STRUCTURE IN THE UNIVERSE AND STELLAR CHEMISTRY.

PREVIOUS STUDIES OF ACTIVE GALACTIC NUCLEI (AGN) SHOW THAT OVER HALF OF ALL AGN SHOW OUTFLOWS FROM THEIR NUCLEAR REGIONS AS EVIDENCED BY BLUE-SHIFTED

REU SITE: RESEARCH EXPERIENCES FOR UNDERGRADUATES IN ASTRONOMY AT CERRO TOLOLO INTER-AMERICAN OBSERVATORY (2012-2016)

THIS PROPOSAL WILL TARGET SCIENCE ANALYSIS FOR THE SOLAR DYNAMICS OBSERVATORY (SDO) SPECIAL INITIATIVE IN HELIOPHYSICS LIVING WITH A STAR SCIENCE.

RETRIEVING THE MOLECULAR COMPOSITION OF PLANET-FORMING MATERIAL: AN ACCURATE NON-LTE RADIATIVE TRANSFER CODE FOR JWST BASED ON THE OBSERVED DISTRIBU

WE PROPOSE TO CARRY OUT TWO SEPARATE GROUND-BASED ASTRONOMICAL OBSERVING PROGRAMS DESIGNED TO BETTER CHARACTERIZE THE LIST OF CANDIDATE EXOPLANET HO

WE PROPOSE TO INVESTIGATE THE RESOLVED VARIATIONS OF THE DUST ABUNDANCE AND PROPERTIES WITHIN AND BETWEEN GALAXIES IN THE NEARBY UNIVERSE TO INFORM CHEMICAL EVOLUTION MODELS CONSTRAIN DUST FORMATION AND DESTRUCTION PROCESSES AND TIMESCALES AND IMPROVE DUST AND GAS MASS ESTIMATES IN THE DISTANT UNIVERSE. WE WILL FIRST ANCHOR ARCHIVAL SPITZER AND HERSCHEL OBSERVATIONS OF NEARBY GALAXIES TO PREVIOUS ALL-SKY OBSERVATIONS WITH IRAS COBE/DIRBE AND PLANCK TO ACCOUNT FOR DIFFUSE DUST EMISSION NOT DETECTED IN SPITZER AND HERSCHEL DUE TO THE NATURE OF THOSE MEASUREMENTS. WE WILL THUS CONSIDERABLY IMPROVE THE CALIBRATION AND LEGACY VALUE OF HERSCHEL AND SPITZER SCIENCE PRODUCTS. WE WILL APPLY AN EXISTING DUST MODEL TO THE SPECTRAL ENERGY DISTRIBUTION (SED) IN THE IMPROVED SPITZER AND HERSCHEL DATA PRODUCTS AND DERIVE MAPS OF THE DUST SURFACE DENSITY PROPERTIES AND ABUNDANCE IN NEARBY GALAXIES WHICH WILL BE MADE PUBLICLY AVAILABLE. BECAUSE FAINT DUST EMISSION IS NOT DETECTED IN INDIVIDUAL PIXELS WE WILL ALSO USE A STACKING ANALYSIS TO MEASURE HOW THE DUST SURFACE DENSITY AND ABUNDANCE (GAS-TO-DUST RATIO G/D) VARY WITH GAS SURFACE DENSITY OVER THE WHOLE SURFACE DENSITY RANGE OF THE ISM INCLUDING THE VERY DIFFUSE ISM (?GAS<A FEW MO PC-2) WHERE DUST DESTRUCTION PROCESSES ARE THE MOST EFFECTIVE. WE WILL DETERMINE HOW THE RELATION BETWEEN DUST ABUNDANCE AND GAS SURFACE DENSITY VARIES WITH METALLICITY AND HUBBLE TYPE AND COMPARE OUR OBSERVATIONAL CONSTRAINTS ON THE DUST SCALING RELATIONS (G/D VS ?GAS METALLICITY AND HUBBLE TYPE) WITH RESOLVED CHEMICAL EVOLUTION MODELS. THIS WILL ALLOW US TO CONSTRAIN DUST FORMATION AND DESTRUCTION PROCESSES AND THEIR ASSOCIATED TIMESCALES. THE DUST SCALING RELATIONS DERIVED IN THE NEARBY UNIVERSE WILL BE APPLICABLE TO THE HIGH-REDSHIFT UNIVERSE AND SUBSTANTIALLY IMPROVE THE ACCURACY OF DUST-BASED GAS MASS ESTIMATES.

REU SITE: RESEARCH EXPERIENCES FOR UNDERGRADUATES (REU) SITE PROGRAM AT KITT PEAK NATIONAL OBSERVATORY

THE AREA OF RESEARCH IDENTIFIED IN SECTION 4 OF MY ORIGINAL IDS PROPOSAL WERE: 1- PREPARATORY OBSERVATIONS. INCL. EVOLUTION OF THE FUNDAMENTAL PLAN

EXECUTE A BALANCED SCIENCE PROGRAM BASED ON DISCIPLINE-SPECIFIC GUIDANCE FROM THE NATIONAL ACADEMIES OF SCIENCES ENGINEERING AND MEDICINE ADMINISTRATION PRIORITIES AND DIRECTION FROM CONGRESS. PARTICIPATE AS A KEY PARTNER AND ENABLER IN THE AGENCY S EXPLORATION INITIATIVE FOCUSING ON SCIENTIFIC RESEARCH OF ON AND FROM THE MOON LUNAR ORBIT MARS AND BEYOND. ADVANCE DISCOVERY IN EMERGING FIELDS BY IDENTIFYING AND EXPLOITING CROSS-DISCIPLINARY OPPORTUNITIES BETWEEN TRADITIONAL SCIENCE DISCIPLINES DEVELOP A DIRECTORATE-WIDE TARGET-USER FOCUSED APPROACH TO APPLIED PROGRAMS INCLUDING EARTH SCIENCE APPLICATIONS SPACE WEATHER PLANETARY DEFENSE AND SPACE SITUATIONAL AWARENESS.

WE PROPOSE TO STUDY LARGE-SCALE SUB-SURFACE FLOWS OF THE SUN DETERMINED FROM SDO DATA ON TIME SCALES OF DAYS TO YEARS IN ORDER TO INVESTIGATE THE LIN

THE INNER FEW ASTRONOMICAL UNITS OF GAS-RICH PROTOPLANETARY DISK ARE ENVIRONMENTS CHARACTERIZED BY A RICH AND ACTIVE GASEOUS CHEMISTRY. PRIMITIVE MAT

REU/RET SITE PROGRAM AT THE NATIONAL SOLAR OBSERVATORY

THE ORIGINS PHYSICAL MECHANISMS AND DIVERSITY OF SUPERNOVAE (SNE) AND OTHER EXPLOSIVE TRANSIENTS REMAIN SHROUDED IN MYSTERY. THE HIGH-CADENCE LIGHTCURVES OF TESS WITH UNPRECEDENTED PRECISION PROVIDES CRITICAL EARLY TIME DATA PROBING A WINDOW THAT

EXECUTE A BALANCED SCIENCE PROGRAM BASED ON DISCIPLINE-SPECIFIC GUIDANCE FROM THE NATIONAL ACADEMIES OF SCIENCES ENGINEERING AND MEDICINE ADMINISTRATION PRIORITIES AND DIRECTION FROM CONGRESS. PARTICIPATE AS A KEY PARTNER AND ENABLER IN THE AGENCY S EXPLORATION INITIATIVE FOCUSING ON SCIENTIFIC RESEARCH OF ON AND FROM THE MOON LUNAR ORBIT MARS AND BEYOND. ADVANCE DISCOVERY IN EMERGING FIELDS BY IDENTIFYING AND EXPLOITING CROSS-DISCIPLINARY OPPORTUNITIES BETWEEN TRADITIONAL SCIENCE DISCIPLINES DEVELOP A DIRECTORATE-WIDE TARGET-USER FOCUSED APPROACH TO APPLIED PROGRAMS INCLUDING EARTH SCIENCE APPLICATIONS SPACE WEATHER PLANETARY DEFENSE AND SPACE SITUATIONAL AWARENESS

GOALS&OBJECTIVES: WE SEEK TO UNDERSTAND WHETHER THE 'NANOFLARE HYPOTHESIS CAN EXPLAIN CORONAL HEATING BY ANALYZING NEW HIGH QUALITY EMPIRICAL DATA AND BY UNDERSTANDING THOSE DATA USING BOTH THEORY AND FORWARD MODELING. DESPITE SEVERAL IMPORTANT STUDIES OVER THE PAST TWO DECADES IT IS NOT YET CLEAR WHETHER THE SMALLEST SCALE EVENTS DELIVER MORE OR LESS POWER TO THE CORONA THAN DO SOLAR FLARES THEMSELVES. THE NUMBER VS. ENERGY DISTRIBUTION OF ENERGETIC EVENTS IS A POWER LAW WHOSE EXPONENT IS TANTALIZINGLY CLOSE TO THE CRITICAL VALUE OF -2. EXACTLY WHERE THE EXPONENT LANDS HAS NOT BEEN CONCLUSIVELY DETERMINED HOWEVER AND THE POWER LAW MAY CHANGE AT THE SMALLEST SCALES (HERE NOISE EFFECTS DOMINATE EXISTING STUDIES SO THEORETICAL ESTIMATES HAVE EXTRAPOLATED FROM LARGER SCALES). WE WILL FOCUS ON THE DISTRIBUTIONS OF THE SMALLEST IMPULSIVE EVENTS VISIBLE WITH SDO/AIA WHICH OFFERS GREATLY IMPROVED SENSITIVITY CADENCE TEMPERATURE COVERAGE AND FOV COMPARED TO PRIOR WORK USING TRACE. THE PROPERTIES OF EACH DETECTED EVENT WILL BE CAREFULLY CATALOGUED USING DIFFERENTIAL EMISSION MEASURE (DEM) ANALYSIS TO INFER TEMPERATURES AND ENERGETICS. IN TANDEM WITH THE AIA DATA ANALYSIS WE WILL CARRY OUT 'SYNTHETIC DATA' ANALYSIS EXERCISES AND FORWARD FITTING USING THE EBTEL AND/OR HYDRAD NUMERICAL MODELS TO IDENTIFY AND CORRECT FOR SYSTEMATIC CROSS-SCALE BIAS IN THE DETECTION ALGORITHMS. OUR MODELING COMPONENT IS A CRITICAL INNOVATION BECAUSE IT ALLOWS US TO UNDERSTAND AND CORRECT SYSTEMATIC SAMPLING EFFECTS THAT COULD SKEW THE SMALL-SCALE TAIL OF THE DISTRIBUTION. THESE EFFECTS INCLUDE BOTH SAMPLING BIAS AND PHYSICAL EFFECTS THAT AFFECT DETECTABILITY OF INDIVIDUAL EVENTS.

IT'S ELEMENTARY: CHEMICAL COMPOSITIONS AND CHARACTERIZATION OF EXOPLANET-HOSTING M-DWARFS USING APOGEE SCIENCE GOALS AND OBJECTIVES: THE DETERMINAT

EXECUTE A BALANCED SCIENCE PROGRAM BASED ON DISCIPLINE-SPECIFIC GUIDANCE FROM THE NATIONAL ACADEMIES OF SCIENCES ENGINEERING AND MEDICINE ADMINISTRATION PRIORITIES AND DIRECTION FROM CONGRESS. PARTICIPATE AS A KEY PARTNER AND ENABLER IN THE AGENCY S EXPLORATION INITIATIVE FOCUSING ON SCIENTIFIC RESEARCH OF ON AND FROM THE MOON LUNAR ORBIT MARS AND BEYOND. ADVANCE DISCOVERY IN EMERGING FIELDS BY IDENTIFYING AND EXPLOITING CROSS-DISCIPLINARY OPPORTUNITIES BETWEEN TRADITIONAL SCIENCE DISCIPLINES DEVELOP A DIRECTORATE-WIDE TARGET-USER FOCUSED APPROACH TO APPLIED PROGRAMS INCLUDING EARTH SCIENCE APPLICATIONS SPACE WEATHER PLANETARY DEFENSE AND SPACE SITUATIONAL AWARENESS

ONE OF THE MAJOR ACHIEVEMENTS OF THE KEPLER MISSION WAS THE DISCOVERY OF TRANSITING CIRCUMBINARY PLANETS. SUCH PLANETS LIKELY FORM IN CIRCUMBINARY DISKS. OBSERVATIONS INDICATE THAT SUCH DISKS MAY FORM MISALIGNED WITH RESPECT TO THE ORBITAL PLANE OF THE CENTRAL BINARY. WE PROPOSE TO FIRST STUDY THE EVOLUTION OF SUCH DISKS FOR A WIDE RANGE OF POSSIBLE INITIAL MASSES AND INCLINATIONS AND FOR A VARIETY OF ECCENTRICITIES OF THE CENTRAL BINARY. FOR SMALL INCLINATIONS EVOLUTION ULTIMATELY TOWARDS COPLANARITY IS EXPECTED. HOWEVER FOR ECCENTRIC ORBIT BINARIES THE EVOLUTION INVOLVES SECULAR TILT OSCILLATIONS TOWARDS AND AWAY FROM COPLANARITY BEFORE COPLANARITY IS ACHIEVED. FOR LARGER INCLINATIONS WE HAVE RECENTLY FOUND THAT AN INITIALLY MODERATELY MISALIGNED CIRCUMBINARY PROTOPLANETARY DISK AROUND AN ECCENTRIC BINARY CAN EVOLVE TO AN ORIENTATION THAT IS PERPENDICULAR TO THE ORBITAL PLANE OF THE BINARY (POLAR ALIGNMENT). WE PROPOSE TO CONTINUE OUR STUDIES OF THE TILT DISK EVOLUTION OF CIRCUMBINARY DISKS. FOR PLANETS FORMED IN SUCH DISKS WE WILL INVESTIGATE THEIR ORBITAL EVOLUTION DUE TO PLANET-DISK AND PLANET-BINARY INTERACTIONS. WE PROPOSE TO INVESTIGATE THESE PROCESSES FOR A RANGE OF BINARY AND DISK PARAMETERS BY MEANS OF ANALYTIC ONE-DIMENSIONAL AND THREE-DIMENSIONAL SIMULATIONS. THE RESULTS WILL PROVIDE INSIGHTS INTO THE ORIGIN AND CURRENT STATE OF CIRCUMBINARY PLANETS.

COLLABORATIVE RESEARCH: SWIFT-SAT: MINIMIZING SCIENCE IMPACT ON LSST AND OBSERVATORIES WORLDWIDE THROUGH ACCURATE PREDICTIONS OF SATELLITE POSITION AND OPTICAL BRIGHTNESS -DUE TO INCREASING NUMBERS OF SATELLITES, PARTICULARLY IN NON-GEOSTATIONARY (NGSO) ORBIT, IMPACTS FROM OPTICAL REFLECTIONS TO KEY ASTRONOMICAL SYSTEMS SUCH AS THE LEGACY SURVEY OF SPACE AND TIME (LSST) ARE ANTICIPATED TO BE PROFOUND WITHOUT MITIGATION. SUCH MITIGATION MAY TAKE SEVERAL FORMS, BUT PREDICTIONS OF SATELLITE LOCATIONS AND BRIGHTNESS WILL LIKELY PLAY A KEY ROLE IN AVOIDANCE OF OPTICAL INTERFERENCE. THIS WORK INCLUDES DEVELOPMENT OF SOFTWARE DESIGNED TO PRODUCE THESE PREDICTIONS BASED UPON OBSERVED TRACKING DATA FOR SATELLITES, AND PRODUCE EXPECTED ERRORS INTRODUCED IN GROUND-BASED ASTRONOMICAL OBSERVATORIES. THIS WILL MAKE BETTER AVOIDANCE OF SUCH ERRORS POSSIBLE. THIS WORK BRINGS TOGETHER A CONSORTIUM OF EXPERTS TO QUANTIFY AND ULTIMATELY MITIGATE IMPACTS ON TWO KEY LSST SCIENCE GOALS AS WELL AS DEVELOP SOFTWARE FOR USE BY GROUND-BASED ASTRONOMERS. THE PIS INTEND TO LEVERAGE A COLLABORATION WITH AEROSPACE CORPORATION TO PRODUCE PREDICTIVE DATA ON SATELLITE BRIGHTNESS AND LOCATION. BRIGHTNESS PREDICTIONS WILL MAKE USE OF A NOVEL TOOL, LUMOS-SAT, THAT ENABLES BIDIRECTIONAL REFLECTANCE DISTRIBUTION FUNCTION (BRDF) FITTING TO BOTH LABORATORY AND ON-ORBIT OBSERVATIONAL DATA. FURTHER, DATA COLLECTED THROUGH A NETWORK OF ENGAGED OBSERVERS AT THE IAU CENTRE FOR THE PROTECTION OF THE DARK AND QUIET SKY FROM SATELLITE CONSTELLATION INTERFERENCE (CPS) SATHUB, AS WELL AS EARLY LSST DATA, WILL BE ANALYZED TO VALIDATE THE ACCURACY OF THE SOFTWARE (?SATCHECKER?) PREDICTIONS. THIS INFORMATION WILL BE USED TO DEVELOP AN ANALYSIS OF ERRORS INTRODUCED BY SATELLITE STREAKS IN LSST OBSERVING PROGRAMS. THIS AWARD REFLECTS NSF'S STATUTORY MISSION AND HAS BEEN DEEMED WORTHY OF SUPPORT THROUGH EVALUATION USING THE FOUNDATION'S INTELLECTUAL MERIT AND BROADER IMPACTS REVIEW CRITERIA.- SUBAWARDS ARE PLANNED FOR THIS AWARD.

IN THEIR FINAL STAGE OF EVOLUTION, ASYMPTOTIC GIANT BRANCH (AGB) STARS INJECT A SUBSTANTIAL AMOUNT OF DUST INTO THE SURROUNDING INTERSTELLAR MEDIUM,

DURING THE FINAL PHASES OF STELLAR EVOLUTION ASYMPTOTIC GIANT BRANCH STARS (AGB;<10 MSUN) BECOME PRODIGIOUS DUST PRODUCERS AND MAY BE THE DOMINANT STELLAR SOURCE OF INTERSTELLAR MEDIUM (ISM) DUST. IN OUR OWN SOLAR SYSTEM ABOUT 90% OF PRESOLAR GRAINS SHOW EVIDENCE FOR AN AGB ORIGIN. THIS IS AT ODDS WITH MODELS OF AGB DUST INPUT THAT SUGGEST THAT AGB STARS MAY ONLY CONTRIBUTE AROUND 2% OF THE ISM DUST IN THE SOLAR NEIGHBORHOOD WITH ISM GRAIN GROWTH AND SUPERNOVAE (SNE) RESPONSIBLE FOR THE REMAINING DUST. NEW RESULTS FROM NITTLER ET AL. (2018) SUGGEST THAT PRESOLAR GRAINS ARE ENRICHED BY MATERIAL THAT MAY HAVE COME FROM A NEARBY ELECTRONCAPTURE SN. THE PROGENITORS OF THESE SNE ARE VERY RARE SUPER-AGB STARS (8-10 MSUN) SUGGESTING THAT OUR SOLAR SYSTEM MAY BE UNUSUAL. DIRECT MEASUREMENTS OF THE WIDE-SCALE DUST INPUT IN A STAR-FORMING SOLAR-METALLICITY ENVIRONMENT DO NOT EXIST BECAUSE MILKY WAY MEASUREMENTS ARE COMPLICATED BY DISTANCE UNCERTAINTIES THAT GAIA CANNOT RESOLVE BECAUSE IT OPERATES AT OPTICAL WAVELENGTHS. AS SUCH COMPREHENSIVE DUST BUDGET SURVEYS HAVE ONLY BEEN POSSIBLE IN THE MAGELLANIC CLOUDS WHERE THE LOW METALLICITY (20-50% SOLAR) SIGNIFICANTLY AFFECTS THE AGB DUST INPUT RENDERING THEM POOR PROXIES FOR THE SOLAR NEIGHBORHOOD. WE PROPOSE TO USE ARCHIVAL SPITZER DATA OF THE NEARBY ANDROMEDA GALAXY (M31) TO IDENTIFY AND CHARACTERIZE DUST PRODUCING STARS. M31 IS THE ONLY MASSIVE L* METAL-RICH GALAXY NEARBY ENOUGH TO RESOLVE STARS PROVIDING A WINDOW INTO THE PHYSICAL PROCESSES THAT SHAPED BOTH OUR OWN HOME IN THE MILKY WAY AND THE ENVIRONMENTS OF MASSIVE GALAXIES THAT DOMINATE REDSHIFT SURVEYS. PRELIMINARY ANALYSIS SHOWS THAT WE CAN IDENTIFY THE DUST PRODUCING STARS IN THE SPITZER DATA WHEN LEVERAGING INFORMATION FROM THE PANCHROMATIC HUBBLE ANDROMEDA TREASURY (PHAT) WHICH IMAGED 1/3 OF M31'S DISK FROM THE UV TO THE NEAR-IR. WHEN COMBINED THE SPITZER DATA REVEAL THE DUSTIEST OBJECTS AND CAN BE USED TO ESTIMATE A GLOBAL DUST INPUT. WE WILL COMPARE THESE RESULTS TO THE ISM DUST MASS DERIVED FROM ARCHIVAL HERSCHEL DATA TO PRODUCE THE FIRST GLOBAL DUST BUDGET FOR A METAL-RICH ENVIRONMENT.

THE HALO OF THE MILKY WAY IS HOME TO A POPULATION OF GASEOUS HIGH-VELOCITY CLOUDS (HVCS) THAT TRACE THE EXCHANGE OF MATTER BETWEEN THE GALAXY AND ITS SURROUNDINGS. HVCS HAVE BEEN STUDIED EXTENSIVELY VIA H I 21 CM EMISSION AND UV METAL-LINE ABSORPTION. HERE WE PROPOSE A THIRD COMPLEMENTARY APPROACH FOR STUDYING HVCS: SURVEYING THEM IN UV LYMAN SERIES H I ABSORPTION USING ALL AGN SPECTRA IN THE FAR-ULTRAVIOLET SPECTROSCOPIC EXPLORER (FUSE) ARCHIVE. THIS H I SURVEY WILL CONSTITUTE A METAL-INDEPENDENT VIEW OF THE BARYONS IN THE GALACTIC HALO AT A LEVEL OVER 1000 TIMES MORE SENSITIVE THAN 21 CM SURVEYS AND IT CAN BE CONDUCTED WITH ARCHIVAL DATA ALONE. 67 AGN ARE AVAILABLE IN THE FUSE ARCHIVES WITH SUITABLE PROPERTIES (S/N>4 AT 977 A) AND THE DATA ARE REDUCED AND READY FOR ANALYSIS.WITH THESE DATA WE WILL CALCULATE HVC SKY COVERING FRACTIONS IN H I ABSORPTION AND CONDUCT HVC METALLICITY MEASUREMENTS IN SIGHTLINES WITH UV METAL ABSORPTION IN HST/COS OR HST/STIS SPECTRA. WE WILL CALCULATE THE GALACTIC H I COLUMN DENSITY DISTRIBUTION FUNCTION (CDDF) THE INCIDENCE OF H I CLOUDS PER UNIT COLUMN DENSITY THAT ENCODES UNDERLYING DENSITY AND IONIZATION VARIATIONS AND IS SENSITIVE TO THE ESCAPING IONIZATION RADIATION FIELD. THE CDDF HAS BEEN MEASURED AT HIGH REDSHIFTS OVER EIGHT ORDERS OF MAGNITUDE OF H I COLUMN DENSITY VIA QUASAR-ABSORPTION LINE EXPERIMENTS. HOWEVER THE GALACTIC H I CDDF HAS UNTIL NOW ONLY BEEN CONSTRAINED AT HIGH H I COLUMN DENSITY WHERE HVCS CAN BE SEEN IN 21CM EMISSION. OUR DETAILED WORK PLAN WILL INVOLVE IDENTIFYING AND MODELING HVC ABSORPTION IN TEN LYMAN SERIES LINES FROM LY GAMMA 972 TO LY MU 917 IN EACH SIGHT LINE IN THE FUSE SAMPLE. THIS WILL CONSTRAIN THE H I CDDF IN THE COLUMN DENSITY RANGE LOG N(H I)~14 TO 18. BY COMBINING WITH THE EXISTING H I CDDF IN 21 CM HVCS IN THE RANGE LOG N(H I)~18 TO 21 FROM THE ALL-SKY GASS SURVEY WE WILL PRODUCE A GLOBAL GALACTIC CDDF COMPLETE OVER SEVEN ORDERS OF MAGNITUDE PROVIDING KEY NEW INFORMATION ON THE DISTRIBUTION OF DIFFUSE GAS IN THE GALACTIC HALO. THIS WILL ALLOW US TO PLACE THE MILKY WAY S HALO IN THE CONTEXT OF THOSE OF EXTERNAL GALAXIES AND TO IDENTIFY THE GALACTIC CONTRIBUTION FROM BOUND GAS IN HALOS TO THE EXTRAGALACTIC CDDF.

SHINE: HELICITY TRANSPORT FROM THE SOLAR INTERIOR TO THE CORONA AND ITS ROLE IN FLARES AND CORONAL MASS EJECTIONS (CMES)

REU SITE: RESEARCH EXPERIENCES FOR UNDERGRADUATES (REU) SITE PROGRAM AT KITT PEAK NATIONAL OBSERVATORY

WE PROPOSE TO DETERMINE STAR FORMATION HISTORIES OF GALAXIES SINCE A REDSHIFT OF 5. IN PARTICULAR, WE WILL MEASURE THE FRACTION OF GALAXIES WHICH EXP

ADVANCED TECHNOLOGY LARGE APERTURE SPACE TELESCOPE: A TECHNOLOGY ROADMAP FOR THE NEXT DECADEMAJOR B

THE ROSES FUNDING OPPORTUNITY GOALS ARE: EXECUTE A BALANCED SCIENCE PROGRAM BASED ON DISCIPLINE-SPECIFIC GUIDANCE FROM THE NATIONAL ACADEMIES OF SCIENCES ENGINEERING AND MEDICINE ADMINISTRATION PRIORITIES AND DIRECTION FROM CONGRESS. PARTICIPATE AS A KEY PARTNER AND ENABLER IN THE AGENCY S EXPLORATION INITIATIVE FOCUSING ON SCIENTIFIC RESEARCH OF ON AND FROM THE MOON LUNAR ORBIT MARS AND BEYOND. ADVANCE DISCOVERY IN EMERGING FIELDS BY IDENTIFYING AND EXPLOITING CROSS-DISCIPLINARY OPPORTUNITIES BETWEEN TRADITIONAL SCIENCE DISCIPLINES DEVELOP A DIRECTORATE-WIDE TARGET-USER FOCUSED APPROACH TO APPLIED PROGRAMS INCLUDING EARTH SCIENCE APPLICATIONS SPACE WEATHER PLANETARY DEFENSE AND SPACE SITUATIONAL AWARENESS.

THE XO PLANET FINDING SYSTEM

MULTI-OBJECTIVE OPTIMAL SCHEDULING FOR SPACE SCIENCE APPLICATIONSWE PROPOSE TO DEVELOP AND ASSESS A

EXECUTE A BALANCED SCIENCE PROGRAM BASED ON DISCIPLINE-SPECIFIC GUIDANCE FROM THE NATIONAL ACADEMIES OF SCIENCES ENGINEERING AND MEDICINE ADMINISTRATION PRIORITIES AND DIRECTION FROM CONGRESS. PARTICIPATE AS A KEY PARTNER AND ENABLER IN THE AGENC

THE ROSES FUNDING OPPORTUNITY GOALS ARE: EXECUTE A BALANCED SCIENCE PROGRAM BASED ON DISCIPLINE-SPECIFIC GUIDANCE FROM THE NATIONAL ACADEMIES OF SCIENCES ENGINEERING AND MEDICINE ADMINISTRATION PRIORITIES AND DIRECTION FROM CONGRESS. PARTICIPATE AS A KEY PARTNER AND ENABLER IN THE AGENCY S EXPLORATION INITIATIVE FOCUSING ON SCIENTIFIC RESEARCH OF ON AND FROM THE MOON LUNAR ORBIT MARS AND BEYOND. ADVANCE DISCOVERY IN EMERGING FIELDS BY IDENTIFYING AND EXPLOITING CROSS-DISCIPLINARY OPPORTUNITIES BETWEEN TRADITIONAL SCIENCE DISCIPLINES DEVELOP A DIRECTORATE-WIDE TARGET-USER FOCUSED APPROACH TO APPLIED PROGRAMS INCLUDING EARTH SCIENCE APPLICATIONS SPACE WEATHER PLANETARY DEFENSE AND SPACE SITUATIONAL AWARENESS.

TELESCOPE SCIENCE INSTITUTEA GENERAL TOOL FOR ASTROPHYSICAL DATA ANALYSISSUMMARY: WE PROPOSE TO DEVE

REU SITE: RESEARCH EXPERIENCE IN OPTICAL-INFRARED ASTRONOMY AT NOIRLAB IN CHILE -THIS PROJECT WILL SUPPORT SIX UNDERGRADUATE STUDENTS PER YEAR FOR A 10 WEEK RESEARCH EXPERIENCE AT NSF FACILITIES AT LA SERENA IN CHILE. THE STUDENTS WILL CARRY OUT MEANINGFUL RESEARCH PROJECTS UNDER THE EXPERT SUPERVISION OF NSF'S NATIONAL OPTICAL-INFRARED ASTRONOMY RESEARCH LABORATORY (NOIRLAB) LARGE AND DIVERSE SCIENTIFIC STAFF. THE STUDENTS WILL HAVE FIRST-HAND EXPERIENCE WITH NOIRLAB'S STATE-OF-THE-ART TELESCOPES AND INSTRUMENTATION AT THE SITE. PARTICIPANTS WILL ALSO ENGAGE IN CULTURAL ACTIVITIES INVOLVING FIELD TRIPS AND INTERACTIONS WITH THEIR CHILEAN COUNTERPARTS FROM THE PRACTICE EN INVESTIGATION EN ASTRONOMIA (PIA) PROGRAM, WHICH OFFERS RESEARCH EXPERIENCES FOR CHILEAN STUDENTS. THE STUDENTS WILL BE RECRUITED BROADLY, FROM ACROSS THE US AND PUERTO RICO, AND FROM INSTITUTIONS THAT ARE DIVERSE IN SIZE AND TYPE, ESPECIALLY THOSE THAT DO NOT COMMONLY OFFER RESEARCH EXPERIENCES. THE STUDENT PROJECTS WILL PRIMARILY MAKE USE OF SCIENCE-READY DATA PRODUCTS AND INVOLVE TOPICS AND TECHNIQUES AT THE FOREFRONT OF ASTROPHYSICS, INCLUDING GALACTIC STRUCTURE, STAR CLUSTERS AND DWARF GALAXIES, STAR FORMATION, THE INTERSTELLAR MEDIUM, TIME DOMAIN, AND LARGE DATA SETS. THE STUDENTS WILL RECEIVE PROFESSIONAL DEVELOPMENT TRAINING PROVIDED BY THE STAFF AT NOIRLAB IN LA SERENA. THIS TRAINING WILL INCLUDE PROFESSIONAL ETHICS, PRESENTATION OF SCIENTIFIC WORK, OPPORTUNITIES AND CAREER PATHS (BOTH IN AND OUT OF ACADEMIA), AND STRATEGIES FOR SUCCESSFUL JOB INTERVIEWS. THIS AWARD REFLECTS NSF'S STATUTORY MISSION AND HAS BEEN DEEMED WORTHY OF SUPPORT THROUGH EVALUATION USING THE FOUNDATION'S INTELLECTUAL MERIT AND BROADER IMPACTS REVIEW CRITERIA.- SUBAWARDS ARE NOT PLANNED FOR THIS AWARD.

DUST IN THE INTERSTELLAR MEDIUM PLAYS A CENTRAL ROLE IN STAR FORMATION AND GALAXY EVOLUTION. WE ARE PROPOSING TO PERFORM A CENSUS OF DUST IN THE LOCA

DYNAMICS OF PLANET-DISK INTERACTIONS WE PROPOSE TO INVESTIGATE SOME THEORETICAL ISSUES CONCERNING PLANET MIGRATION AND ECCENTRICITY EVOLUTION THROUG

EXECUTE A BALANCED SCIENCE PROGRAM BASED ON DISCIPLINE-SPECIFIC GUIDANCE FROM THE NATIONAL ACADEMIES OF SCIENCES ENGINEERING AND MEDICINE ADMINISTRATION PRIORITIES AND DIRECTION FROM CONGRESS. PARTICIPATE AS A KEY PARTNER AND ENABLER IN THE AGENCY S EXPLORATION INITIATIVE FOCUSING ON SCIENTIFIC RESEARCH OF ON AND FROM THE MOON LUNAR ORBIT MARS AND BEYOND. ADVANCE DISCOVERY IN EMERGING FIELDS BY IDENTIFYING AND EXPLOITING CROSS-DISCIPLINARY OPPORTUNITIES BETWEEN TRADITIONAL SCIENCE DISCIPLINES. DEVELOP A DIRECTORATE-WIDE TARGET-USER FOCUSED APPROACH TO APPLIED PROGRAMS INCLUDING EARTH SCIENCE APPLICATIONS SPACE WEATHER PLANETARY DEFENSE AND SPACE SITUATIONAL AWARENESS.

NASA IAA FOR THE NATIONAL SOLAR OBSERVATORY -THIS IS THE GOVERNING COOPERATIVE AGREEMENT FOR AN INTERAGENCY AGREEMENT WITH NASA. NATIONAL SOLAR OBSERVATORY WILL CARRY OUT ACTIVITIES PER VARIOUS SPECIFIC AGREEMENTS. THIS AWARD REFLECTS NSF'S STATUTORY MISSION AND HAS BEEN DEEMED WORTHY OF SUPPORT THROUGH EVALUATION USING THE FOUNDATION'S INTELLECTUAL MERIT AND BROADER IMPACTS REVIEW CRITERIA.- SUBAWARDS ARE NOT PLANNED FOR THIS AWARD.

WE PROPOSE TO INVESTIGATE THREE THEORETICAL ISSUES INVOLVING PLANET-DISK INTERACTIONS. THE FIRST PROJECT IS TO CONTINUE OUR INVESTIGATIONS OF PLANET

LAYING THE FOUNDATION FOR A COMPREHENSIVE VIEW OF TRANSITING EXOPLANETS WITH THE GALACTIC BULGE SURVEY

WE REQUEST SUPPORT FROM THE NASA ASTROPHYSICS DATA ANALYSIS PROGRAM TO QUANTIFY THE MASS RETURN FROM EVOLVED STARS IN THE MAGELLANIC CLOUDS (MCS). AT

EXECUTE A BALANCED SCIENCE PROGRAM BASED ON DISCIPLINE-SPECIFIC GUIDANCE FROM THE NATIONAL ACADEMIES OF SCIENCES ENGINEERING AND MEDICINE ADMINISTRATION PRIORITIES AND DIRECTION FROM CONGRESS. PARTICIPATE AS A KEY PARTNER AND ENABLER IN THE AGE

COMPUTATIONALLY EFFICIENT ADAPTIVE WAVEFRONT CONTROL FOR CORONAGRAPHY USING ALGORITHMIC DIFFERENTIATION

REU SITE PROGRAM AT THE NATIONAL SOLAR OBSERVATORY

THIS PROPOSAL TARGETS SUB-ELEMENT B.4.1 - OPEN DATA - DEVELOPMENT ELEMENT (ODDE). MAGNETIC FLUX SYNOPTIC CHARTS ARE CRITICAL FOR RELIABLE MODELING OF

21-LWSTM21_2-0005 HELIOPHYSICS LIVING WITH A STAR TOOLS AND METHODS

NATIONAL OPTICAL ASTRONOMY OBSERVATORY SCIENCE RESEARCH SUPPORT

WE PROPOSE A PILOT STUDY TO DEVELOP PIPELINE TOOLS THAT WILL BE USED TO SEARCH FOR NEOS WITH THE DARK ENERGY CAMERA (DECAM), A FACILITY-CLASS WIDE-FI

"THE ULTRAVIOLET SPACE OBSERVATORY (USO): A CONCEPT STUDY AND TECHNOLOGY ROADMAP FOR FUTURE SPECTROS

INTERGOVERNMENTAL MOBILITY ASSIGNMENT

EXECUTE A BALANCED SCIENCE PROGRAM BASED ON DISCIPLINE-SPECIFIC GUIDANCE FROM THE NATIONAL ACADEMIES OF SCIENCES ENGINEERING AND MEDICINE ADMINISTRATION PRIORITIES AND DIRECTION FROM CONGRESS. PARTICIPATE AS A KEY PARTNER AND ENABLER IN THE AGENC

IRES: U.S.-INDIA SUMMER PROGRAM IN ASTROPHYSICS

SUPERNOVAE (SN) AND ACTIVE GALACTIC NUCLEI (AGN) VARY ON TIMESCALES OF HOURS TO MONTHS AND ARE STILL SHROUDED IN MYSTERY. WE PROPOSE A LARGE K2 PROGRAM TO MONITOR ON THE ORDER OF 10 000 BRIGHT GALAXIES IN EACH OF CAMPAIGN C14 C15 AND C16 WHICH SHOULD YIELD IN TOTAL MORE THAN 15 GREAT LIGHT CURVES (LCS) OF SUPERNOVAE. IN KEPLER GO PROGRAMS WE HAVE IDENTIFIED TO DATE 3 SN IA (OLLING ET AL. 2015) 2 SN IIP (GARNAVICH ET AL. 2016; TUCKER ET AL. SUBMITTED) AND 1 SN IIN/IA-CSM (GARNAVICH ET AL. IN PREP.). WE ALSO FOUND THAT ~4% OF OUR GALAXIES DISPLAY AGN ACTIVITY WITH VARIABILITY AT>0.001% LEVEL (SHAYA ET AL 2015). IN K2 CAMPAIGN C3 C5 C6 C8 AND C10 WE IDENTIFIED MORE THAN 15 SNE THREE OF WHICH WE SPECTROSCOPICALLY CLASSIFIED. ANALYSIS OF THE K2 DATA IS ONGOING. WITH OUR PROGRAM WE PLAN TO A) DETERMINE THE TYPES OF COMPANIONS TO PROGENITORS OF SNE USING FEATURES IN THE EARLY BREAKOUT (T<4 DAYS) LCS; B) EXPLORE THE EXPLOSION PHYSICS OF SN ESPECIALLY SN IA USING SUBTLE FEATURES DURING THEIR RISE (T<20 DAYS); C) IMPROVE THE CALIBRATION OF SN IA AS STANDARD CANDLES FOR MEASURING DISTANCES HO AND DARK ENERGY USING K2 LCS OF UNPRECEDENTED DETAIL; AND D) ADD SIGNIFICANT KNOWLEDGE TO THE VIRTUALLY UNEXPLORED VERY LOW-EDDINGTON REGIME OF AGN. THERE IS AN ONGOING CONTROVERSY OVER THE BASIC PHYSICS OF ONE OF THE KEY TOOLS IN COSMOLOGY THE SN IA STANDARD CANDLE. DO SNE IA GRADUALLY REACH CRITICAL MASS VIA ACCRETION FROM A COMPANION STAR OR DOES IT MERGE WITH ANOTHER WD? IF A WHITE DWARF HAD BEEN ACCRETING MASS FROM A COMPANION STAR AS THE EJECTA REACHES THE COMPANION A SHOCK WOULD FORM WITH OBSERVABLE OPTICAL EMISSION (KASEN 2010). THE EMISSION WOULD BE SHORT AND STRONGEST FROM CERTAIN VIEWING ANGLES REQUIRING RAPID CADENCE FOR SEVERAL SNE BEFORE DEFINITIVE CONCLUSIONS CAN BE REACHED. FOR THE 3 SN IA DISCOVERED BY KEPLER MONITORING OF ~500 GALAXIES (OLLING ET AL. 2015) NO SIGNATURES OF A COMPANION WERE FOUND AND TIGHT CONSTRAINTS WERE PLACED. WITH A LARGER SAMPLE WE CAN DETERMINE THE STATISTICS FOR THE TWO POSSIBLE CHANNELS THAT TRIGGER SN IA. MEANWHILE FEATURES DUE TO THE DIFFERENT EXPLOSION PHYSICS (DETONATION DEFLAGRATION INWARDS-MOVING DIFFUSION WAVES ETC) OF IA AND CORE COLLAPSE SNE WILL ALSO BE REVEALED. K2 WILL ALLOW FOR THE FIRST TIME TO TEST MODELS MORE COMPLICATED THAN SIMPLE "EXPANDING FIREBALLS." WE WILL UNDERTAKE A MAJOR CONCURRENT GROUND-BASED EFFORT TO OBSERVE THE ENTIRE FIELD EVERY OTHER DAY USING SKYMAPPER ATLAS AND DECAM. WE WILL ALSO COORDINATE MULTI-COLOR PHOTOMETRY AND SPECTRA TO CLASSIFY DISCOVERED TRANSIENTS USING LICK GEMINI AND KECK. IN CAMPAIGN C5 AND C6 WE SUCCESSFULLY IDENTIFIED 4 SNE WITH DECAM OBSERVATIONS OF WHICH WE CLASSIFIED 2 WITH GEMINI SPECTRA AS SN IA. THESE DATA COUPLED WITH HIGH PRECISION 30 MINUTE K2 DATA WILL HAVE ENORMOUS LEGACY VALUE. METHODS: WE HAVE DEVELOPED AND PROVEN A HIGHLY SUCCESSFUL DETRENDING METHOD THAT SIMULTANEOUSLY SOLVES FOR THE SAWTOOTH PATTERN CAUSED BY POINTING MOTION AND FOR THE COEFFICIENTS OF VECTORS FROM PRINCIPAL COMPONENT ANALYSIS OF TARGETS ON THE SAME CHANNEL. THIS ITERATIVE TECHNIQUE PERMITS US TO DEFINE APERTURE SIZES BETTER SUITED TO THIS PROBLEM AND TO MAKE EXCELLENT CORRECTIONS FOR SENSITIVITY VARIATIONS ON ALL TIME SCALES. TO PROPERLY CORRECT SN LIGHT CURVES THE TECHNIQUE IS APPLIED TO THE QUIET TIME BEFORE THE EVENT AND THEN EXTRAPOLATED TO THE END OF THE CAMPAIGN. REFERENCES: GARNAVICH ET AL. 2016 APJ 820 23 (KEGS PAPER) GARNAVICH ET AL. APJ IN PREP. (KEGS PAPER) KASEN 2010 AJ 708 1025 OLLING ET AL. 2015 NATURE 521 332 (KEGS PAPER) SHAYA ET AL. 2015 AJ 150 188 (KEGS PAPER) TUCKER ET AL. SUBMITTED (KEGS PAPER)

THE ORIGINS SPACE TELESCOPE (OST) IS AN EVOLVING CONCEPT FOR THE FAR-INFRARED SURVEYOR MISSION AND THE SUBJECT OF ONE OF THE FOUR SCIENCE AND TECHNOLOGY DEFINITION STUDIES SUPPORTED BY NASA HEADQUARTERS TO PREPARE FOR THE 2020 ASTRONOMY AND ASTROPHYSICS DECADAL SURVEY. THE ORIGINS SPACE TELESCOPE WILL CHARACTERIZE EXOPLANETS THE MOST DISTANT GALAXIES NEARBY GALAXIES AND THE MILKY WAY AND THE OUTER REACHES OF OUR SOLAR SYSTEM. THE GOAL OF THE STUDY IS TO CREATE A MISSION CONCEPT THAT IS SCIENTIFICALLY COMPELLING AND EXECUTABLE IN THE 2030 S. THIS PROPOSED GRANT WILL PROVIDE PARTIAL SUPPORT FOR THE PI MARGARET MEIXNER TO WORK ON THIS STUDY WHILE ON SABBATICAL FROM HER DUTIES AT STSCI. THERE HAVE BEEN MANY ACCOMPLISHMENTS ON THE OST STUDY TO DATE. HOWEVER THIS COMING YEAR IS A VERY CRITICAL YEAR WITH COMPLETION OF THE INTERIM REPORT ON MISSION CONCEPT 1 THE CREATION OF MISSION CONCEPT 2 ON LIMITED RESOURCES AND THE FINAL REPORT. MEIXNER IS ONE OF THE COMMUNITY CHAIRS FOR THE STUDY AND HAS A RESPONSIBILITY TO LEAD THE STDT AND WORK WITH THE STUDY CENTER TO COMPLETE THE REPORTS FOR NASA HQ. HER GOAL IS TO COMPLETE THE FINAL REPORT WHILE ON SABBATICAL.

SUPERNOVAE SN AND ACTIVE GALACTIC NUCLEI AGN VARY ON TIMESCALES OF HOURS TO MONTHS AND ARE STILL SHROUDED IN MYSTERY. WE PROPOSE A LARGE K2 PROGRAM TO MONITOR 2500 BRIGHT GALAXIES IN CAMPAIGN C12 WHICH SHOULD YIELD 2 5 GREAT LIGHT CURVES LCS OF SUPERNOVAE. IN KEPLER GO PROGRAMS WE IDENTIFIED 3 SN IA OLLING ET AL 2015 2 SN IIP GARNAVICH ET AL IN PRESS TUCKER ET AL SUBMITTED AND 1 SN IIN IA CSM GARNAVICH ET AL IN PREP. WE ALSO FOUND THAT 4 OF OUR GALAXIES DISPLAY AGN ACTIVITY WITH VARIABILITY AT 0.001 LEVEL SHAYA ET AL 2015. IN K2 CAMPAIGNS C3 C5 AND C6 WE IDENTIFIED 3 3 AND 2 SNE RESPECTIVELY TWO OFWHICH WERE SPECTROSCOPICALLY CLASSIFIED. ANALYSIS OF THE K2 DATA IS ONGOING. WITH OUR PROGRAM WE PLAN TO DETERMINE THE TYPES OF COMPANIONS TO PROGENITORS OF SNE USING FEATURES IN THE EARLY BREAKOUT T 4 DAYS LCS EXPLORE THE EXPLOSION PHYSICS OF SN ESPECIALLY SN IA USING SUBTLE FEATURES DURING THEIR RISE T 20 DAYS IMPROVE THE CALIBRATIONOF SN IA AS STANDARD CANDLES FOR MEASURING DISTANCES HO AND DARK ENERGY USING K2 LCS OF UNPRECEDENTED DETAIL AND ADD SIGNIFICANT KNOWLEDGE TO THE VIRTUALLY UNEXPLORED VERY LOW EDDINGTON REGIME OF AGN.THERE IS AN ONGOING CONTROVERSY OVER THE BASIC PHYSICS OF ONE OF THE KEY TOOLS IN COSMOLOGY THE SN IA STANDARD CANDLE. DO SNE IA GRADUALLY REACH CRITICAL MASS VIA ACCRETION FROM A COMPANION STAR OR DOES IT MERGE WITH ANOTHER WD? IF A WHITE DWARF HAD BEEN ACCRETING MASS FROM A COMPANION STAR AS THE EJECTA REACHES THE COMPANION A SHOCK WOULD FORM WITH OBSERVABLE OPTICAL EMISSION KASEN 2010. THE EMISSION WOULD BE SHORT AND STRONGEST FROM CERTAIN VIEWING ANGLES REQUIRING RAPID CADENCE FOR SEVERAL SNE BEFOREDEFINITIVE CONCLUSIONS CAN BE REACHED. FOR THE 3 SN IA DISCOVERED BY KEPLER MONITORING OF 500 GALAXIES OLLING ET AL 2015 NO SIGNATURES OF A COMPANION WERE FOUND AND TIGHT CONSTRAINTS WERE PLACED. WITH A LARGER SAMPLE WE CAN DETERMINE THE STATISTICS FOR THE TWO POSSIBLE CHANNELS THAT TRIGGER SN IA. MEANWHILE FEATURES DUE TO THE DIFFERENT EXPLOSION PHYSICS DETONATION DEFLAGRATION INWARDS MOVING DIFFUSION WAVES ETC OF IA AND CORE COLLAPSE SNE WILL ALSO BE REVEALED. K2 WILL ALLOW FOR THE FIRST TIME TO TEST MODELSMORE COMPLICATED THAN SIMPLE EXPANDING FIREBALLS.OUR PROGRAM WILL IMPROVE THE SN IA CALIBRATION FOR DISTANCE MEASUREMENTS. BY DETERMINING CORRELATIONS AMONG THE KEY PARAMETERS NEEDED FOR DISTANCE FITTING LIGHT CURVE WIDTH MAXIMUM AND THE EXPLOSION TIME ON THE SCALE OF MINUTES RATHER THAN DAYS THIS PROGRAM WILL IMPROVE THE PRECISION OF DISTANCES AND HENCE THE CONSTRAINTS ON DARK ENERGY.WE WILL UNDERTAKE A MAJOR CONCURRENT GROUND-BASED EFFORT TO OBSERVE THE ENTIRE FIELD EVERY OTHER DAY USING SKYMAPPER ATLAS AND DECAM. WE WILL ALSO COORDINATE MULTI COLOR PHOTOMETRY AND SPECTRA TO CLASSIFY DISCOVERED TRANSIENTS USING LICK GEMINI AND KECK. IN CAMPAIGN C5 AND C6 WE SUCCESSFULLY IDENTIFIED 4 SNE WITH DECAM OBSERVATIONS OF WHICH WE CLASSIFIED 2 WITH GEMINI SPECTRA AS SN IA. THESE DATA COUPLED WITH HIGH PRECISION 30 MINUTE K2 DATA WILL HAVE ENORMOUS LEGACY VALUE.METHODSWE HAVE DEVELOPED AND PROVEN A HIGHLY SUCCESSFUL DETRENDING METHOD THAT SIMULTANEOUSLY SOLVES FOR THE SAWTOOTH PATTERN CAUSED BY POINTING MOTION AND FOR THE COEFFICIENTS OF VECTORS FROM PRINCIPAL COMPONENT ANALYSIS OF TARGETS ON THE SAME CHANNEL. THIS ITERATIVE TECHNIQUE PERMITS US TO DEFINE APERTURE SIZES BETTER SUITED TO THIS PROBLEM AND TO MAKE EXCELLENT CORRECTIONS FOR SENSITIVITY VARIATIONS ON ALL TIME SCALES. TO PROPERLY CORRECT SN LIGHT CURVES THE TECHNIQUE IS APPLIED TO THE QUIET TIME BEFORE THE EVENT AND THEN EXTRAPOLATED THROUGH TO THE END OF THE CAMPAIGN.

A MAJOR GOAL IN CONTEMPORARY ASTROPHYSICS IS TO EXTEND THE STUDY OF STELLAR ATMOSPHERES TO THE MUCH COOLER ATMOSPHERES OF GAS-GIANT EXTRASOLAR PLANETS. ONE KEY PATHWAY IS THE IDENTIFICATION OF FREE-FLOATING SUBSTELLAR OBJECTS THAT NOT ONLY SHARE COMMON TEMPERATURES WITH EXOPLANETS BUT ALSO COMMON MASSES AND THUS SURFACE GRAVITIES. IN RECENT YEARS SEARCHES FOR EVER COLDER FREE-FLOATING OBJECTS HAVE STEADILY PUSHED THE CENSUS TO EVER LOWER MASSES AND FINALLY INTO THIS LONG-SOUGHT PLANETARY-MASS REGIME (5-15 JUPITER MASSES; Y DWARFS). THE EMPIRICAL BACKBONE OF THE EXPLORATION OF THESE NEW SUBSTELLAR SAMPLES IS THE ACCURATE MEASUREMENT OF DISTANCES VIA TRIGONOMETRIC PARALLAXES. DISTANCES ALLOW US TO MAKE EMPIRICAL SEQUENCES OF ABSOLUTE MAGNITUDE VERSUS COLOR AND SPECTRAL TYPE TO COMPARE TO BETTER STUDIED NORMAL BROWN DWARFS AS WELL AS PROVIDING ABSOLUTE BOLOMETRIC FLUXES AND THEREBY LUMINOSITIES AND TEMPERATURES. HOWEVER UNLIKE SIMPLE PHOTOMETRY OR SPECTROSCOPY PARALLAX MEASUREMENTS ARE TIME CONSUMING AND PRONE TO LARGE SYSTEMATIC ERRORS WHEN ATTEMPTED BY COMBINING DATA FROM MULTIPLE TELESCOPES AND BANDPASSES. SPITZER/IRAC IS POISED TO DELIVER THE DEFINITIVE SAMPLE OF PARALLAX DISTANCES FOR THE COLDEST BROWN DWARFS. IT IS THE ONLY FACILITY CAPABLE OF MEASURING HIGH-PRECISION ASTROMETRY EFFICIENTLY FOR A LARGE SAMPLE OF SUCH FAINT SUBSTELLAR OBJECTS AS VALIDATED BY OUR PAST WORK. SPITZER WAS NEVER INTENDED TO DELIVER HIGH QUALITY ASTROMETRY BUT USING OUR CUSTOM BUILT ASTROMETRIC PIPELINE WE HAVE SUCCESSFULLY PRODUCED THE FIRST PRECISE IRAC ASTROMETRY AND MEASURED DISTANCES FOR A SMALL INITIAL SAMPLE OF THE COLDEST BROWN DWARFS (DUPUY&KRAUS 2013). WE SHOWED THAT IN SPITE OF THE SEEMINGLY SUBTLE SPECTRAL CHANGES FROM T8 TO Y0 (ONLY 2 SUBTYPES) THE MEAN EFFECTIVE TEMPERATURE PLUMMETS BY ALMOST A FACTOR OF 2 FROM ~700 K FOR T8 DWARFS TO ~400 K FOR Y0 DWARFS. EVEN IN THIS SMALL SAMPLE WE FOUND SOME OBJECTS THAT SEEMED TO DEFY THE EXPECTATION THAT LATER SPECTRAL TYPE CORRESPONDS TO COOLER TEMPERATURE. THIS MAY POINT TO COMPLEXITY IN THE ATTEMPT TO SPECTRAL TYPE PLANETARY MASS OBJECTS AS OTHER PARAMETERS LIKE GRAVITY OR NONEQUILIBRIUM CHEMISTRY COULD BECOME JUST AS IMPORTANT AS TEMPERATURE. HOWEVER A SAMPLE LARGER THAN ONE OR TWO OBJECTS PER SPECTRAL TYPE BIN IS REQUIRED TO MAKE ANY DEFINITIVE STATEMENTS ABOUT PHYSICAL TRENDS. WE PROPOSE A COMPREHENSIVE STUDY OF THE COLDEST KNOWN BROWN DWARFS BY MEASURING ACCURATE DISTANCES FROM SPITZER PARALLAXES. WE WILL USE ALL DATA IN THE SPITZER ARCHIVE SUITABLE FOR PARALLAXES TO PERFORM A HOMOGENEOUS ANALYSIS OF A COMPLETE SAMPLE OF THE LATEST T AND Y DWARFS. OUR PROPOSED WORK WILL ROUGHLY TRIPLE THE SAMPLE SIZE AND FILL IN MAJOR GAPS AT THE T9.5 AND>Y0 SPECTRAL TYPES (~300-350 K) THAT PRODUCED SOME OF THE MOST PUZZLING RESULTS IN OUR PREVIOUS WORK. THE LONGER TIME BASELINE WILL ENABLE>3X MORE PRECISE PARALLAX MEASUREMENTS THAN IS POSSIBLE FROM THE GROUND FOR SIMILARLY FAINT OBJECTS. THE RESULTING EMPIRICAL SEQUENCES OF ABSOLUTE MAGNITUDE WILL PROVIDE A TOUCHSTONE FOR COMPARING BOTH MODELS AND DATA E.G. FROM DIRECTLY IMAGED EXOPLANETS. WE WILL ALSO USE THE ABSOLUTE FLUXES TO DERIVE BOLOMETRIC LUMINOSITIES FOR OUR SAMPLE. COMBINING THESE WITH WELL-ESTABLISHED MODEL RADII WILL RESULT IN ROBUST TEMPERATURE DETERMINATIONS THAT WILL ALLOW DEEPER SCRUTINY OF WHETHER TEMPERATURE OR A MORE COMPLEX MIX OF PHYSICAL PROPERTIES DRIVES SPECTRAL VARIATIONS IN THE PLANETARY MASS REGIME. FINALLY OUR ASTROMETRIC MONITORING WILL NATURALLY ALLOW US TO EXAMINE THE POPULATION S KINEMATICS AND THE LONG TIME BASELINE WILL ALLOW A NOVEL SEARCH FOR LOWER MASS COMPANIONS VIA NONLINEAR PERTURBATIONS. OUR PROPOSED WORK WILL RESULT IN A DEFINITIVE BENCHMARK SAMPLE FOR BOTH THE BROWN DWARF AND EXOPLANET COMMUNITIES PROVIDING CONTEXT FOR CURRENT AND FUTURE EFFORTS TO CHARACTERIZE BROWN DWARFS DIRECTLY IMAGED PLANETS AND THE COOL TRANSITING PLANETS PROBED BY SECONDARY ECLIPSE MEASUREMENTS.

THE PRINCIPAL INVESTIGATOR (PI) PROPOSES TO ANALYZE ARCHIVAL SPITZER WARM MISSION EXOPLANET OBSERVATIONS WITH THE GOAL OF IMPROVING THE PRECISION OF

THE WFIRST-AFTA MISSION CURRENTLY INCLUDES THE PROVISION FOR A HIGH CONTRAST IMAGING INSTRUMENT WITH A PRIMARY GOAL OF DISCOVERING NEW, LOW MASS EXOP

THE PHYSICAL QUANTITIES CALCULATED FROM HMI FILTERGRAMS EXHIBIT SMALL BUT IMPORTANT SYSTEMATIC ERRORS RELATED TO THE SDO ORBITAL VELOCITY THAT SHOW UP IN LINE-OF-SIGHT (LOS) DOPPLER VELOCITY V LOS MAGNETIC FIELD M AND THE VECTOR FIELD B. RESULTS SHOW A C. 1% NOT-QUITE-LINEAR SCALE ERROR IN VELOCITY AND SOMEWHAT LARGER 24- AND 12-HOUR PERIODIC VARIATIONS IN REPORTED MAGNETIC FIELD VALUES. THOUGH SMALL THEY ARE SYSTEMATIC AND HINDER SOME ANALYSES OF SOME SOLAR QUANTITIES THAT DEPEND ON FRAME-TO-FRAME DIFFERENCES IN THE REPORTED MAGNETIC FIELD SUCH AS ENERGY AND HELICITY TRANSPORT THROUGH THE

THE ZWICKY TRANSIENT FACILITY (ZTF) IS ON TRACK TO TRANSFORM THE FIELD OF TIDAL DISRUPTION EVENTS (TDES). IN THE FIRST 2.5 YR. OF ZTF SURVEY OPERATIONS (ZTF-I) WE HAVE DETECTED 25 TDES. WITH THE FINAL 5-YEAR SAMPLE FROM ZTF-I+ZTF-II

WE PROPOSE A LARGE K2 PROGRAM TO MONITOR GALAXIES WITH SUPPLEMENTARY GROUND-BASED RESOURCES TO DISCOVER FOLLOW-UP AND ANALYZE ANY SNE IMAGED BY K2 IN C17 C18 AND C19. IN C16 WE DISCOVERED 18 CONFIRMED SNE AND WE EXPECT TO FIND ~40 SNE IN CYCLE 6 CAMPAIGNS. IN KEPLER GO PROGRAMS WE IDENTIFIED 3 SN IA (OLLING ET AL. 2015) 2 SN IIP (GARNAVICH ET AL. 2016; TUCKER ET AL. SUBMITTED) AND 1 SN IIN/IA-CSM (GARNAVICH ET AL. IN PREP.) AND SEVERAL GALAXIES EXHIBITING AGN ACTIVITY. IN BACKWARD-FACING K2 CAMPAIGNS (C3-C15) WE IDENTIFIED 27 SNE (6 SPECTROSCOPICALLY CLASSIFIED) INCLUDING KSN2015K THE FASTEST BRIGHT SN TO DATE (REST ET AL. 2018). ANALYSIS OF K2 DATA IS ONGOING.

TRANSFORMING OUR KNOWLEDGE OF AGN WINDS WITH XRISM

MY RESEARCH HAS FOCUSED ON THE LARGE AND SMALL MAGELLANIC CLOUDS (LMC AND SMC) WITH THE OVER-ARCHING GOAL TO UNDERSTAND DUST EVOLUTION IN THESE TWO GALAXIES. I HAVE BOTH LED AND PARTICIPATED IN SEVERAL LARGE OBSERVATIONAL SURVEYS OF THE LMC AND SMC USING SPITZER AND HERSCHEL.

THE GOAL OF THIS PROPOSAL IS TO EXPLORE THE INCIDENCE OF STELLAR FLARING IN A SET OF SIMULTANEOUS GALEX-KEPLER DATA TO EXPAND OUR UNDERSTANDING OF HOW RADIATION IF DISTRIBUTED IN DIFFERENT STELLAR FLARES. THE PROPOSED PROJECT WILL DRASTICALLY ENLARGE (BY A FACTOR OF APPROXIMATELY 100) THE NUMBER OF SIMULTANEOUSLY OBSERVED MULTI-WAVELENGTH STELLAR FLARES. FROM THESE FLARES THE RADIATED ENERGY FRACTIONATIONS IN THE OPTICAL AND NUV BAND PASSES AND THEIR DISTRIBUTION WILL BE DETERMINED. THIS IS IMPORTANT FOR TESTING THE CONTINUATION OF THE POWER-LAW DISTRIBUTION OF FLARE OCCURRENCE RATE AND EXAMINING FLARE HEATING MODELS UNDER A RANGE OF DIFFERENT ENERGY INPUT REGIMES. OPTICAL FLARES ARE EASIER TO OBSERVE WITH BROAD BAND WHITE-LIGHT FILTERS AND SENSITIVE SPACE MISSIONS YET SHORTER WAVELENGTHS ARE MORE RESPONSIVE TO THE IMPULSIVE NATURE OF THE FLARE AND REVEAL MORE ABOUT THE TIMESCALES OVER WHICH THE FLARE ENERGY INPUT OCCURS. SHORTER WAVELENGTHS ARE ALSO MORE IMPACTFUL FOR THE STELLAR ENVIRONMENT INCLUDING PENETRATING DEEPER INTO AN EXOPLANET S ATMOSPHERE. MULTI-WAVELENGTH MEASUREMENTS ENABLE ESTIMATION OF THE FLARE INCREASE AT NUV WAVELENGTHS FOR FLARES WITHOUT NUV MEASUREMENTS; THE RESULTS OF THIS WORK WILL ENABLE EXTENSION TO ALL OF THE FLARES OBSERVED BY KEPLER AND TESS.

COLLABORATIVE RESEARCH: SHINE: STUDY OF LONG-TERM VARIABILITY OF SOLAR CHROMOSPHERIC ACTIVITY IN MULTIPLE SOLAR CYCLES

OBSCURING OUTFLOWS ARE REMARKABLY DIFFERENT FROM THE COMMONLY SEEN WARM-ABSORBER OUTFLOWS IN ACTIVE GALACTIC NUCLEI (AGN). THEY EXHIBIT LARGE COLUMNS OF HIGH-VELOCITY GAS CLOSE TO THE BLACK HOLE.

PR 76-8032-20 INVESTIGATING MAGNETIC FLUX ROPE EMERGENCE AS THE SOURCE OF FLARING ACTIVITY IN DELTA-SPOT

MASS-LOSING EVOLVED STARS AND IN PARTICULAR ASYMPTOTIC GIANT BRANCH (AGB) STARS AND RED SUPERGIANT (RSG) STARS ARE EXPECTED TO BE THE MAJOR PRODUCERS OF DUST IN GALAXIES. THIS DUST WILL HELP FORM PLANETARY SYSTEMS AROUND FUTURE GENERATIONS OF STARS. OUR ADAP PROGRAM TO MEASURE THE MASS LOSS FROM THE AGB AND RSG STARS IN THE MAGELLANIC CLOUDS IS NEARING COMPLETION AND WE WISH TO EXTEND THIS SUCCESSFUL STUDY TO THE GALACTIC BULGE OF THE MILKY WAY GALAXY. METALLICITY SHOULD DETERMINE THE AMOUNT OF ELEMENTS AVAILABLE TO CONDENSE DUST IN THE STAR'S OUTFLOW SO EVOLVED STARS OF DIFFERING METALLICITIES SHOULD HAVE DIFFERING MASS-LOSS RATES. BUILDING UPON OUR WORK ON EVOLVED STARS IN THE MAGELLANIC CLOUDS WE WILL COMPARE THE MASS-LOSS RATES FROM AGB AND RSG STARS IN THE OLDER AND POTENTIALLY MORE METAL-RICH BULGE TO THE MASS-LOSS RATES OF AGB AND RSG STARS IN THE MAGELLANIC CLOUDS WHICH HAVE LOWER METALLICITY MAKING FOR AN INTERESTING CONTRAST. IN ADDITION THE GALACTIC BULGE LIKE THE CLOUDS IS LOCATED AT A WELLDETERMINED DISTANCE (~8 KPC) THEREBY REMOVING THE DISTANCE AMBIGUITIES THAT PRESENT A MAJOR UNCERTAINTY IN DETERMINING MASS-LOSS RATES AND LUMINOSITIES FOR EVOLVED STARS. TO MODEL PHOTOMETRIC OBSERVATIONS OF OUTFLOWING DUST SHELLS AROUND EVOLVED STARS WE HAVE CONSTRUCTED THE GRID OF RED SUPERGIANT AND ASYMPTOTIC GIANT BRANCH MODELS (GRAMS; SARGENT ET AL 2011; SRINIVASAN ET AL 2011) USING THE RADIATIVE TRANSFER CODE 2DUST (UETA AND MEIXNER 2003). OUR STUDY WILL APPLY THESE MODELS TO THE LARGE PHOTOMETRIC DATABASE OF SOURCES IDENTIFIED IN THE SPITZER SPACE TELESCOPE GLIMPSE SURVEY OF THE MILKY WAY AND ALSO TO THE VARIOUS INFRARED SPECTRA OF BULGE AGB AND RSG STARS FROM SPITZER ISO ETC. WE HAVE ALREADY MODELED A FEW GALACTIC BULGE EVOLVED STARS WITH GRAMS AND WE WILL USE THESE RESULTS AS THE FOUNDATION FOR MODELING A LARGE AND REPRESENTATIVE SAMPLE OF GALACTIC BULGE EVOLVED STARS IDENTIFIED AND MEASURED PHOTOMETRICALLY BY GLIMPSE. WE WILL USE OUR GRAMS GRID EXPANDING AS NECESSARY TO ENABLE MODELING OF THE HIGHER METALLICITY EVOLVED STARS OF THE GALACTIC BULGE ALONG WITH MODELS OF OTHER TYPES OF STARS SUCH AS YSOS (ROBITAILLE ET AL 2006) TO IDENTIFY THE EVOLVED STARS IN THE GLIMPSE SAMPLE OF THE GALACTIC BULGE. WE WILL USE THESE WELL-TESTED GRAMS MODELS WHICH WE HAVE ALREADY EXTENSIVELY APPLIED TO STUDY POPULATIONS OF MASS LOSING EVOLVED STARS IN THE MAGELLANIC CLOUDS TO FIT THE SPECTRAL ENERGY DISTRIBUTIONS (SEDS; PLOTS OF EMITTED POWER VERSUS WAVELENGTH) OF GLIMPSE GALACTIC BULGE SOURCES IDENTIFIED AS RSG STARS AND OXYGEN-RICH (O-RICH) CARBON-RICH (C-RICH) AND EXTREME AGB STARS. THIS MODELING WILL YIELD STELLAR LUMINOSITIES AND MASS-LOSS RATES AS WELL AS GENERAL DUST CHEMISTRY (O-RICH VERSUS C-RICH) AND OTHER ESSENTIAL CHARACTERISTICS OF THE DUST PRODUCED BY EVOLVED STARS IN THE GALACTIC PLANE. OUR ONGOING MAGELLANIC CLOUD AND PROPOSED MILKY WAY GALACTIC BULGE EVOLVED STAR STUDIES WILL LAY THE GROUNDWORK FOR FUTURE STUDIES OF EVOLVED STARS IN OTHER NEARBY GALAXIES USING DATA FROM THE JAMES WEBB SPACE TELESCOPE AND OTHER PLANNED MISSIONS.

A KEY COMPONENT OF THE CURRENT WFIRST-AFTA MISSION IS HIGH CONTRAST IMAGING OF PLANETS AND DEBRIS DISKS AROUND NEARBY STARS. IT IS EXPECTED THAT THE

WITH THE END OF THE HERSCHEL MISSION AND NO IMMEDIATE SUCCESSOR AT FAR-INFRARED WAVELENGTHS, IT IS IMPERATIVE TO EXTRACT AS MUCH INFORMATION AS POSSI

CONFERENCE: WINDOWS ON THE UNIVERSE: ESTABLISHING THE INFRASTRUCTURE FOR A COLLABORATIVE MULTI-MESSENGER ECOSYSTEM -THE PROPOSED CONFERENCE, TO BE HELD ON OCTOBER 16-18 IN TUCSON AZ, WILL BRING TOGETHER GOVERNMENT AGENCIES AND EXPERT SCIENTISTS IN THE FIELD OF MULTI-MESSENGER ASTRONOMY (MMA) ELECTROMAGNETIC FOLLOW-UP. SESSIONS WILL FOCUS ON IDENTIFYING PATHWAYS THAT INCREASE THE COORDINATION OF FOLLOW-UP MMA CAMPAIGNS, REDUCING OPERATIONAL REDUNDANCY ACROSS THE NETWORK OF GROUND- AND SPACE-BASED OBSERVATORIES, AND FOSTERING COLLABORATION IN THE MMA COMMUNITY. THE COMMUNITY WILL BE INVITED TO REVIEW THE CURRENT STATE OF FOLLOW-UP RESOURCES, REPORT ON EXISTING COLLABORATIONS AND PARTNERSHIPS, AND IDENTIFY POTENTIAL OBSTACLES TO SUCCESS. THE CONFERENCE WILL DEVELOP CONCRETE IDEAS THAT WILL BE DISSEMINATED WITHIN A PUBLIC WHITE PAPER. THE FINDINGS OF THE CONFERENCE WILL HELP DEVELOP THE SCOPE OF AN FY2024 NSF SOLICITATION DEDICATED TO FUNDING COORDINATION INFRASTRUCTURE AND EFFORTS AMONG THE FOLLOW-UP COMMUNITY. THIS PROPOSAL REQUESTS FUNDING TO HOST THE WORKSHOP AND TO SUPPORT PARTICIPANT ATTENDANCE ACROSS MULTIPLE FIELDS IN THE MMA COMMUNITY. ALL CONFERENCE PARTICIPANTS ARE REQUIRED TO READ AND AGREE TO THE ISEE CODE OF CONDUCT THAT OUTLINES EXPECTATIONS FOR BEHAVIOR AND CONFIDENTIAL AND NON-CONFIDENTIAL REPORTING OPTIONS FOR ANYONE WHO EXPERIENCES MISCONDUCT. WITH GRAVITATIONAL-WAVE AND PARTICLE DETECTORS NOW ROUTINELY OBSERVING EVENTS THROUGH NEW WINDOWS UPON OUR DYNAMIC UNIVERSE, WE HAVE ENTERED THE ERA OF MULTI-MESSENGER ASTRONOMY. WE HAVE ADVANCED RESOURCES TO BOTH IDENTIFY THE ELECTROMAGNETIC COUNTERPARTS OF MULTI-MESSENGER EVENTS AND THEN MONITOR AND CHARACTERIZE THEIR EVOLUTION. THIS ACTIVITY REQUIRES COORDINATION OF THE FULL RANGE OF AVAILABLE TELESCOPES AND THEIR CAPABILITIES. WHILE THE SCIENTIFIC POTENTIAL IS STAGGERING, FUTURE CAMPAIGNS WILL BE RESOURCE-INTENSIVE, EXPENSIVE, AND REQUIRE CONSIDERABLE COORDINATION, COLLABORATION, AND COMMUNICATION AMONG THE COMMUNITIES IN ORDER TO DELIVER EFFECTIVE SCIENCE. MOTIVATED TO FOSTER EFFECTIVE MULTI-MESSENGER FOLLOW-UP, ORGANIZERS WILL INVITE THE INTERNATIONAL OBSERVING COMMUNITY TO PARTICIPATE IN AN OPEN WORKSHOP. ORGANIZERS WILL ASK THE WORKSHOP PARTICIPANTS TO CONCEPTUALIZE COMMUNITY STRATEGIES AND METHODS OF TACKLING DATA SHARING - I.E., TELESCOPE POINTING PLANS, BOTH PLANNED AND EXECUTED, OBSERVATION OUTCOMES, AND CALIBRATED DATA ETC. FURTHERMORE, WE ASK THE WORKSHOP PARTICIPANTS TO IDENTIFY PATHWAYS WHICH WILL INCENTIVIZE COORDINATION, COLLABORATION, PARTNERSHIP, AND COLLEGIALITY WITHIN THE MMA COMMUNITY. THIS PROPOSAL REQUESTS FUNDING TO HOST A THREE-DAY WORKSHOP, LIMITED IN NUMBER TO NO MORE THAN 90 PEOPLE. THE REQUESTED FUNDING WOULD SUPPORT THE COSTS OF A MEETING VENUE (INCLUDING HYBRID CAPABILITY, PROVIDE TRAVEL SUPPORT FOR A SUBSET OF THE PARTICIPANTS, AND MEALS FOR ALL ATTENDEES. THIS AWARD REFLECTS NSF'S STATUTORY MISSION AND HAS BEEN DEEMED WORTHY OF SUPPORT THROUGH EVALUATION USING THE FOUNDATION'S INTELLECTUAL MERIT AND BROADER IMPACTS REVIEW CRITERIA.

GOALS&OBJECTIVES THE PROPOSED RESEARCH IS A CONTINUATION AND COLLABORATION OF AN EXISTING ONGOING PROJECT TO STUDY EXTREME GAMMA-RAY BURSTS WITH THE

THE SOLAR SYSTEM IS HOME TO THE ONLY KNOWN INHABITED PLANET AND THE HISTORY OF ITS PLANETS PROVIDES INSIGHTS INTO PLANETARY HABITABILITY. WE WILL PRO

LAST YEAR THE PRINCIPAL INVESTIGATOR (PI) AND OTHERS PRESENTED AT SPIE-MARSEILLE A NEW 2-DIMENSIONAL PIXEL-PHASE APERTURE-FLUX CORRECTION FOR IRAC

22-ROMAN22-0090 SPQR: SPECTROSCOPIC PROBES OF QUANTITATIVE REIONIZATION

STSCI WILL PARTNER WITH MARSHALL SPACE FLIGHT CENTER AND ITT TO DEVELOP A TECHNOLOGY PLAN TO MATURE ADVANCED NORMAL INCIDENCE MIRRORS TO A TECHNOLOGY

WE PROPOSE TO DO A CALIBRATION STUDY OF VARIABLE STARS IN THE KEPLER FIELD WHICH WILL BE ENABLE US T

A COMPREHENSIVE, HOMOGENEOUS CHEMICAL ABUNDANCE ANALYSIS OF PLANETARY HOST STARS DISCOVERED BY KEPLER IS PROPOSED. PRECISE STELLAR PARAMETERS (EFFECT

SPACE TELESCOPE SCIENCE INSTITUTEHOW ARE THE WARM- HOT INTERGALACTIC MEDIUM AND G

MARCO CHIABERGE / SPACE TELESCOPE SCIENCE INSTITUTE MEASURING THE DISTANCE OF THE ABSORBER IN NGC7582 WE PROPOSE TO PERFORM 4 SUZAKU OBSERVATION OF 2

WE SEEK SUPPORT TO HOMOGENEOUSLY REDUCE AND ANALYZE ARCHIVAL SPITZER/IRS SPECTRA FOR A SAMPLE OF 147

'BACKYARD WORLDS: BINARIES' -- DISCOVERING BENCHMARK BROWN DWARFS THROUGH CITIZEN SCIENCE

THE FERMI TELESCOPE&#039;S LAT INSTRUMENT HAS FOUND A SAMPLE OF HIGHLY RELATIVISTIC GRBS, WHICH MAY BE AMONG THE MOST ENERGETIC BURSTS EVER DISCOVERE

STAR-FORMING GALAXIES HOST POPULATIONS OF NEWLY FORMED MASSIVE STARS THAT EMIT THE PEAK OF THEIR RADIATION IN THE ULTRAVIOLET (UV). SUCH RADIATION IS

THE CITIZEN CATE (CONTINENTAL-AMERICA TELESCOPE ECLIPSE) EXPERIMENT TO OBSERVE THE 2017 GREAT AMERICAN ECLIPSE

THE ULTRAVIOLET/OPTICAL TELESCOPE (UVOT) ON THE NEIL GEHRELS SWIFT OBSERVATORY HAS BEEN USED FOR AN ENORMOUS VARIETY OF SCIENCE TOPICS BEYOND ITS ORIGINAL PURPOSE OF DETECTING GAMMA RAY BURSTS. AS WE HAVE USED IT TO ANALYZE NEARBY GALAXIES WE HAVE DETERMINED THAT THE CALIBRATION IS INSUFFICIENT TO ACCURATELY MEASURE THE BRIGHTNESS OF THESE EXTENDED SOURCES. WE WILL THEREFORE USE EXISTING UVOT DATA TO IMPROVE THE CALIBRATION AND APPLY IT TO THE SOLV (SWIFT OBSERVATIONS OF THE LOCAL VOLUME) SURVEY WHICH IS IMAGING 465 LOCAL GALAXIES. THE NEWLY-CALIBRATED UVOT DATA WHEN COMBINED WITH ARCHIVAL IMAGING WILL ALLOW US TO MODEL THE SPECTRAL ENERGY DISTRIBUTIONS OF EACH GALAXY REVEALING INFORMATION INCLUDING THEIR STELLAR MASSES STAR FORMATION HISTORY AND THE SHAPE OF THEIR DUST ATTENUATION CURVE. THIS INFORMATION WILL CONTRIBUTE TO OUR UNDERSTANDING OF THE FORMATION AND EVOLUTION OF DWARF GALAXIES WHICH IN TURN WILL INFORM THEORIES FOR THE GROWTH OF STRUCTURE AT SMALL SCALES. THIS ADDRESSES THE NASA SCIENCE MISSION DIRECTORATE BIG QUESTION "HOW DID WE GET HERE?" WHICH SEEKS TO UNDERSTAND HOW THE UNIVERSE TRANSITIONED FROM THE BIG BANG TO THE PLANETS STARS AND GALAXIES WE SEE TODAY.

CONFERENCE: BUILDING BRIDGES: TOWARD A UNIFIED, SUSTAINABLE, OPEN, AND SCALABLE CYBERINFRASTRUCTURE ECOSYSTEM IN ASTRONOMY -ASTRONOMY IS ENTERING A NEW ERA DEFINED BY UNPRECEDENTED DATA VOLUMES, INCREASINGLY COMPLEX ANALYSES, AND THE NEED FOR COLLABORATION AT A GLOBAL SCALE. YET THE TOOLS, DATA SERVICES, AND COMPUTATIONAL INFRASTRUCTURE REQUIRED TO UNLOCK THESE SCIENTIFIC OPPORTUNITIES REMAIN FRAGMENTED AND INCONSISTENTLY SUPPORTED. THIS LIMITS THE COMMUNITY?S ABILITY TO FULLY EXPLOIT DISCOVERIES FROM MAJOR OBSERVATORIES AND SPACE MISSIONS, AND RISKS DUPLICATING EFFORTS RATHER THAN BUILDING ON SHARED STRENGTHS. A UNIFIED, SUSTAINABLE, AND SCALABLE CYBERINFRASTRUCTURE (CI) ECOSYSTEM WOULD TRANSFORM HOW ASTRONOMERS ACCESS, ANALYZE, AND SHARE DATA, ACCELERATING DISCOVERY, FOSTERING COLLABORATION, AND ENSURING THAT PUBLICLY FUNDED SCIENCE YIELDS ITS MAXIMUM BENEFIT TO SOCIETY. THE WORKSHOP DESCRIBED IN THIS PROPOSAL WILL BRING TOGETHER THE COMMUNITY?S TECHNICAL EXPERTISE, INSTITUTIONAL LEADERSHIP, AND AGENCY PARTNERS TO CHART A PATH TOWARD THAT VISION. THE PROPOSED THREE DAY WORKSHOP WILL CONVENE SOFTWARE DEVELOPERS, DATA AND ARCHIVE MANAGERS, CI SERVICE PROVIDERS, AND REPRESENTATIVES FROM NSF, NASA, DOE, AND OTHER KEY STAKEHOLDERS. DRAWING ON THE RECOMMENDATIONS OF ASTRO2020, PETABYTES TO SCIENCE, AND THE FUTURE OF ASTRONOMICAL DATA INFRASTRUCTURE, PARTICIPANTS WILL IDENTIFY INSTITUTIONAL AND STRUCTURAL BARRIERS TO COLLABORATION, EXAMINE GOVERNANCE, POLICY, AND SUPPORT MODELS, AND EXPLORE HOW TO ADAPT AND INTEGRATE EXISTING INTEROPERABLE SOLUTIONS INTO A COHESIVE ECOSYSTEM. SESSIONS WILL FOCUS ON SUMMARIZING USE CASES, ASSESSING CURRENT CI ASSETS, EVALUATING MODELS FROM OTHER DISCIPLINES, AND DRAFTING AN INITIAL STRATEGIC ROADMAP. THE OUTCOME WILL BE A WHITE PAPER WITH ACTIONABLE RECOMMENDATIONS, A DRAFT GOVERNANCE AND SUSTAINABILITY FRAMEWORK, AND A PRIORITIZED IMPLEMENTATION PLAN FOR ADVANCING A UNIFIED ASTRONOMICAL CI. THIS AWARD REFLECTS NSF'S STATUTORY MISSION AND HAS BEEN DEEMED WORTHY OF SUPPORT THROUGH EVALUATION USING THE FOUNDATION'S INTELLECTUAL MERIT AND BROADER IMPACTS REVIEW CRITERIA.- SUBAWARDS ARE NOT PLANNED FOR THIS AWARD.

WE WILL USE THE ULTRAVIOLET/OPTICAL TELESCOPE (UVOT) ON THE NEIL GEHRELS SWIFT OBSERVATORY TO OBSERVE FIVE RECENTLY-DISCOVERED DWARF GALAXIES IN THE LOCAL VOLUME. THESE TINY GALAXIES ARE REPRESENTATIVE OF THE BUILDING BLOCKS OF LARGER GALAXIES; UNDERSTANDING THEM ADDRESSES THE NASA SCIENCE MISSION DIRECTORATE BIG QUESTION "HOW DID WE GET HERE?" WHICH SEEKS TO UNDERSTAND HOW THE UNIVERSE TRANSITIONED FROM THE BIG BANG TO THE PLANETS STARS AND GALAXIES WE SEE TODAY. WE WILL COMBINE NEW OBSERVATIONS IN THE UV FILTERS WITH ARCHIVAL IMAGING TO MODEL THE SPECTRAL ENERGY DISTRIBUTIONS OF EACH TINY GALAXY REVEALING INFORMATION INCLUDING THEIR STELLAR MASSES STAR FORMATION HISTORY AND THE SHAPE OF THEIR DUST ATTENUATION CURVE. THIS INFORMATION WILL CONTRIBUTE TO OUR UNDERSTANDING OF THE FORMATION AND EVOLUTION OF DWARF GALAXIES WHICH IN TURN WILL INFORM THEORIES FOR THE GROWTH OF STRUCTURE AT SMALL SCALES.

PRIMORDIAL SOLAR SYSTEM ICES1. DESCRIPTION OF KEY RESEARCH OBJECTIVES THE DISTANT KUIPER BELT OBJECT

FEATURE EXTRACTION TOOLS FOR EXPLORATORY ANALYSIS OF REMOTE-SENSING SOLAR OBSERVATIONS

WE PROPOSE TO BUILD A FRAMEWORK FOR THEP CORONAL AUTOMATED ANALYSIS OF SHOCKS AND WAVES (CASHEW). THE PROPOSED WORK ADDRESSES THE NASA HELIOPHYSICS GUEST INVESTIGATORS SUB-ELEMENT B.4.1: OPEN DATA-DEVELOPMENT ELEMENT (ODDE) IN SUPPORT OF THE CURRENT HELIOPHYSICS SYSTEM OBSERVATORY OPERATING MISSIONS . IT WILL COMBINE ANALYSIS OF NASA HELIOPHYSICS SYSTEM OBSERVATORY DATA PRODUCTS AND RELEVANT DATA-DRIVEN MODELS INTO AN AUTOMATED SYSTEM FOR THE CHARACTERIZATION OF CORONAL WAVES AND SHOCKS AND THE EVALUATION OF THEIR CAPABILITY TO ACCELERATE SEPS. CORONAL MASS EJECTIONS (CMES) ARE ONE OF THE MAIN PHENOMENA THAT MODIFY SPACE WEATHER IN THE HELIOSPHERE. AMONG OTHER EFFECTS DURING THEIR HELIOSPHERIC PROPAGATION THEY ROUTINELY DRIVE COLLISIONLESS SHOCKS WHICH IN TURN MAY PRODUCE SIGNIFICANT FLUXES OF SOLAR ENERGETIC PARTICLES (SEPS). RECENT STUDIES HAVE USED EXTREME UV (EUV) OBSERVATIONS TO SHOW THE CONNECTION OF CORONAL EUV WAVES TO METRIC RADIO TYPE II BURSTS IN THE CORONAL PHASES OF CMES. THIS SIGNIFIES THAT CME-DRIVEN SHOCKS CAN EXIST LOW IN THE CORONA AND MAY ALREADY ACCELERATE SEPS AT THEIR VERY INITIAL STAGES. CHARACTERIZING CORONAL SHOCKS HAS ONLY BECOME POSSIBLE THROUGH REMOTE MEASUREMENTS FROM INSTRUMENTS ON THE SOHO STEREO AND SDO SPACECRAFT. EUV IMAGING WITH THE ATMOSPHERIC IMAGING ASSEMBLY(AIA) INSTRUMENT ON SDO HAS PROVED PARTICULARLY USEFUL FOR DETECTING LARGE-SCALE SHORT-LIVED CORONAL BRIGHT FRONTS WHICH COMBINED WITH RADIO OBSERVATIONS HOLDS GREAT PROMISE FOR EARLY CME-DRIVEN SHOCK CHARACTERIZATION CAPABILITY. THIS CHARACTERIZATION CAN FURTHER BE AUTOMATED AND RELATED TO MODELS OF PARTICLE ACCELERATION TO PRODUCE ESTIMATES OF PARTICLE FLUXES EARLY IN EVENTS. THE CASHEW FRAMEWORK WILL BE EXTENSIVELY TESTED AND VALIDATED ON A REPRESENTATIVE LIST OF CORONAL BRIGHT FRONT EVENTS. SOME OF THE SPECIFIC SCIENTIFIC QUESTIONS THAT CAN BE ADDRESSED THROUGH ANALYSES OF THE PROPOSED DATA PRODUCTS ARE 1) TO WHAT ENERGIES CAN CORONAL SHOCKS ACCELERATE SOLAR ENERGETIC PARTICLES? 2) HOW DOES CORONAL SHOCK ACCELERATION EFFICIENCY VARY WITH TIME AND LOCATION? 3) WHAT REMOTE OBSERVABLES ARE RELEVANT FOR DETERMINATION OF SHOCK ACCELERATION EFFICIENCY? THE PRODUCTS OF THE PROPOSED WORK WILL ENABLE AND FACILITATE FUTURE STUDIES OF CORONAL SHOCK WAVE PROPERTIES AS WELL AS THEIR INFLUENCE ON SEP PRODUCTION AND HELIOSPHERIC CONNECTIVITY. THE CASHEW FRAMEWORK AND ITS RESULTS WILL BE MADE FREELY AVAILABLE ONLINE FOR RESEARCHERS TO USE VIA THE NASA SOLAR DATA ANALYSIS CENTER. THIS PROPOSAL IS RELEVANT TO THE NRC S CURRENT DECADAL SURVEY OF SOLAR AND SPACE PHYSICS AND ITS KEY SCIENCE GOAL 1. DETERMINE THE ORIGINS OF THE SUN'S ACTIVITY AND PREDICT THE VARIATIONS IN THE SPACE ENVIRONMENT . IT WILL ENABLE RESEARCH RELEVANT TO NASA'S STRATEGIC GOAL TO UNDERSTAND THE SUN AND ITS INTERACTIONS WITH THE EARTH AND THE SOLAR SYSTEM AND TO THE FOLLOWING NASA HELIOPHYSICS SCIENCE OBJECTIVES: OPEN THE FRONTIER TO SPACE ENVIRONMENTAL PREDICTION: UNDERSTAND THE FUNDAMENTAL PHYSICAL PROCESSES OF THE SPACE ENVIRONMENT FROM THE SUN TO EARTH AND SAFEGUARD THE JOURNEY OF EXPLORATION: MAXIMIZE THE SAFETY AND PRODUCTIVITY OF HUMAN AND ROBOTIC EXPLORERS BY DEVELOPING THE CAPABILITY TO PREDICT THE EXTREME AND DYNAMIC CONDITIONS IN SPACE.

WE WILL USE THE SPITZER ARCHIVAL DATA FROM THE SURVEYING THE AGENTS OF A GALAXY S EVOLUTION (SAGE) L

SUMMARY: THE SCIENTIFIC GOAL OF THE KEPLER MISSION IS TO EXPLORE THE STRUCTURE AND DIVERSITY OF PLAN

EXECUTE A BALANCED SCIENCE PROGRAM BASED ON DISCIPLINE-SPECIFIC GUIDANCE FROM THE NATIONAL ACADEMIES OF SCIENCES ENGINEERING AND MEDICINE ADMINISTRATION PRIORITIES AND DIRECTION FROM CONGRESS. PARTICIPATE AS A KEY PARTNER AND ENABLER IN THE AGENCY S EXPLORATION INITIATIVE FOCUSING ON SCIENTIFIC RESEARCH OF ON AND FROM THE MOON LUNAR ORBIT MARS AND BEYOND. ADVANCE DISCOVERY IN EMERGING FIELDS BY IDENTIFYING AND EXPLOITING CROSS-DISCIPLINARY OPPORTUNITIES BETWEEN TRADITIONAL SCIENCE DISCIPLINES. DEVELOP A DIRECTORATE-WIDE TARGET-USER FOCUSED APPROACH TO APPLIED PROGRAMS INCLUDING EARTH SCIENCE APPLICATIONS SPACE WEATHER PLANETARY DEFENSE AND SPACE SITUATIONAL AWARENESS.

SPACE TELESCOPE SCIENCE INSTITUTE IDENTIFICATION OF THERMAL COMPONENT IN GRB PROMPT EMISSION: A NEW

ENHANCING THE CAPABILITIES OF CLEDB AN OPEN SOURCE CORONAL VECTOR MAGNETIC FIELD INVERSION TOOL FOR THE HELIOPHYSICS COMMUNITY

SUPPORT FOR CONFERENCES, SYMPOSIA, WORKSHOPS OR OTHER MEETINGS FOR THE NATIONAL OPTICAL ASTRONOMY OBSERVATORY (NOAO)

ADVANCING THE NEW RADIO-LOUD AGN UNIFICATION SCHEME WITH FERMI. WE PROPOSE TO USE FERMI OBSERVATIONS TO ENHANCE A NEW COMPREHENSIVE DATABASE OF RADIO

THE EXOASTEROIDS CITIZEN SCIENCE PROJECT - DISCOVERING INFRARED OUTBURSTS WITH WISE

SUBSURFACE ZONAL AND MERIDIONAL FLOWS FROM RECONSTRUCTED MDI DOPPLERGRAMS SCIENCE GOALS AND OBJECTIVES: THE PROPOSED WORK WILL PROVIDE A UNIQUE DATA SET OF ZONAL AND MERIDIONAL FLOWS IN THE UPPER CONVECTION ZONE USING CONTINUOUSLY AVAILABLE LOW-TELEMETRY DOPPLERGRAMS FROM MICHELSON DOPPLER IMAGER (MDI) INSTRUMENT ON BOARD SOLAR AND HELIOSPHERIC OBSERVATORY. THIS WOULD BE A UNIQUE DATA SET FOR THE SOLAR PHYSICS COMMUNITY SINCE THE CONTINUOUS MDI OBSERVATIONS HAVE NEVER BEEN USED TO PRODUCE SUBSURFACE FLOWS USING RING-DIAGRAM (RD) TECHNIQUE. THE OBJECTIVE IS TO INFER SUBSURFACE HORIZONTAL FLOWS USING THE RING-DIAGRAM TECHNIQUE ONE OF THE MOST SUCCESSFUL TOOLS OF LOCAL HELIOSEISMIC ANALYSIS. THIS METHOD HAS BEEN WIDELY USED TO MEASURE THE FLOWS USING HIGH-RESOLUTION DOPPLERGRAMS FROM GONG MDI AND HMI. HOWEVER FOR RING ANALYSIS THE OBSERVATIONS FROM MDI HAVE BEEN SUITABLE ONLY DURING THE "DYNAMICS PROGRAM" WHICH NORMALLY OCCURRED ABOUT 2 MONTHS IN A YEAR. DUE TO TELEMETRY LIMITATIONS THE DATA FROM OTHER PERIODS WERE DOWN-SAMPLED TRUNCATED AT OUTER SOLAR LIMB AND DOWNLOADED IN LOWER RESOLUTION WHICH IS NOT SUITABLE FOR STANDARD RING ANALYSIS. AS A RESULT RD ANALYSIS USING MDI DATA CAN BE CARRIED OUT INFREQUENTLY ONLY DURING THE 2-MONTH PERIOD IN A YEAR ALTHOUGH MDI OBSERVATIONS ARE AVAILABLE CONTINUOUSLY OVER A PERIOD OF 15 YEARS COVERING TWO MINIMUM AND ONE MAXIMUM PERIODS OF SOLAR ACTIVITY. THUS OUR AIM IS TO USE THE CONTINUOUSLY AVAILABLE LOW-TELEMETRY MDI DATA FROM THE LOW-ACTIVITY PERIOD BEFORE CYCLE 23 THROUGH THE RISING PHASE OF CYCLE 24. THIS WILL ALLOW US TO PRODUCE CONTEMPORARY DATA SETS OF ZONAL AND MERIDIONAL FLOWS IN THE UPPER CONVECTION ZONE FOR THE COMPLETE SOLAR CYCLE 23. NOTE THAT THE FLOWS FROM GONG ARE AVAILABLE FROM JUNE 2001 AND DO NOT COVER THE LOW-ACTIVITY AND RISING PHASE OF CYCLE 23. METHODOLOGY: WE WILL USE MDI SPHERICAL HARMONIC (SH) TIME SERIES FROM JSOC TO RECONSTRUCT SEVERAL 30 BY 30 DEGREE PATCHES AROUND CENTRAL MERIDIAN AND EQUATOR. USE OF THIS SH TIME SERIES HAS SEVERAL ADVANTAGES FIRST IT HAS BEEN GENERATED FROM THE CORRECTED VELOCITY IMAGES (DISTORTION APODIZATION ETC.) AND SECONDLY A SMOOTH TRANSITION NEAR THE SURFACE LAYERS CAN BE PERFORMED BY APPLYING SPECIFIC FILTERS TO THE SH TIME SERIES IN SPHERICAL GEOMETRY. RECONSTRUCTION OF VELOCITY IMAGES USING THE SH COEFFICIENT TIME SERIES (INVERSE SH DECOMPOSITION) WILL BE CARRIED OUT WITH THE EXISTING TIME-DISTANCE PIPELINE DEVELOPED BY US AT NATIONAL SOLAR OBSERVATORY. THIS PIPELINE IS WELL TESTED AND VALIDATED BY MEASURING DEEP MERIDIONAL FLOW PROPERTIES. THESE BIG RING PATCHES (30 DEGREE IN DIAMETER AS OPPOSED TO 15 DEGREE PATCHES USED IN THE STANDARD RING DIAGRAM) WILL BE SUBSEQUENTLY USED TO INFER SUBSURFACE FLOW TO A DEPTH OF 30 MM BY PERFORMING CUSTOM RING ANALYSIS. IT SHOULD BE NOTED THAT OUR DATA PRODUCT THE MERIDIONAL FLOW AND ITS TEMPORAL VARIATIONS AT DIFFERENT DEPTHS OVER 15 YEARS WILL PROVIDE AN ADDITIONAL INDEPENDENT DATA SET TO COMPARE WITH MEASUREMENTS OBTAINED FROM THE TIME-DISTANCE TECHNIQUE. AVAILABILITY OF THIS DATA PRODUCT WILL ALLOW INTERESTED RESEARCH TEAMS TO INVESTIGATE SOLAR CYCLE AND LONG-TERM VARIATIONS OF FLOWS AND DYNAMICS OF THE UPPER CONVECTION ZONE OVER THE WHOLE MDI TIME EPOCH IN CONTRAST TO THOSE AVAILABLE OVER A LIMITED PERIOD OF ONLY TWO MONTHS A YEAR. IN SUMMARY WE PLAN TO GENERATE NEW DATA PRODUCTS FROM THE CONTINUOUS MDI OBSERVATIONS SPANNING A PERIOD OF ABOUT 15 YEARS. THESE PRODUCTS INCLUDE: (I) ZONAL AND MERIDIONAL FLOWS AS A FUNCTION OF THE LATITUDE DEPTH AND TIME (II) CUSTOM DATA CUBES IN AND AROUND WELL-KNOWN LARGE ACTIVE REGIONS FOR BETTER INVESTIGATION OF FLOW PATTERN AROUND THEM AND (III) RECONSTRUCTED DOPPLERGRAMS FOR THE ENTIRE DURATION OF MDI OBSERVATIONS. THESE DATA PRODUCTS WILL ENHANCE THE USAGE OF MDI DOPPLERGRAMS. ALL THESE DATA PRODUCTS WILL BE AVAILABLE TO THE PUBLIC.

HUBBLE WEEKS ONE AND TWO--A PILOT OUTREACH MINI-PROPOSAL IN ORDER TO INCREASE PUBLIC AWARENESS OF HUBBLE SPACE TELESCOPE SERVICING MISSION 4 (SM4) A

COLLABORATIVE RESEARCH: TESTING THE LAMBDA COLD DARK MATTER PARADIGM WITH DWARF SATELLITES OF LOW-MASS GALAXIES

BEYOND THE KUIPER BELT EDGETHE KUIPER BELT IS THE DE-FACTO OUTER EDGE OF THE SOLAR SYSTEM, WITH THE EXCEPTION OF ONE EXTREMELY UNUSUAL OBJECT, SEDNA

HIRMES-ENABLED SCIENCE ALIGNS CLOSELY WITH NASA S STRATEGIC PLAN TO DISCOVER HOW THE UNIVERSE WORKS EXPLORE HOW IT BEGAN AND EVOLVED AND SEARCH FOR PLANETS. HIRMES COMBINATION OF SENSITIVITY WAVELENGTH RANGE AND SPECTRAL RESOLVING POWER PROVIDES A CRITICAL NEW CAPABILITY. OVER THE COURSE OF 10 MILLION YEARS ACCRETION DISKS AROUND PRE-MAIN SEQUENCE STARS TRANSFORM FROM GAS-RICH REMNANTS OF STAR FORMATION INTO YOUNG PLANETARY SYSTEMS. THE PRIMARY PLANET-FORMING REGION IN THESE PROTOPLANETARY DISKS IS LOCATED WITHIN 20 ASTRONOMICAL UNITS AU OF THE SYSTEM S CENTER. THIS REGION IS CHARACTERIZED BY A MIXTURE OF WARM AND COLD GAS DUST AND ICE AND HAS BEEN ANALYZED USING A RANGE OF MOLECULAR AND ATOMIC LINES AND SOLID-STATE FEATURES IN THE MID- TO FAR-INFRARED. HOWEVER TO DELVE MORE DEEPLY TOWARD UNDERSTANDING PLANET FORMATION AND THE CREATION OF PLANETARY ATMOSPHERES REQUIRES THE HIGH-RESOLUTION MID- TO FAR-INFRARED (IR) SPECTROSCOPY HIRMES PROVIDES. HIRMES IS DESIGNED TO PERFORM DETAILED STUDIES OF IMPORTANT DISK CONSTITUENTS: WATER VAPOR AND ICE THESE MATERIALS PLAY A CRITICAL ROLE IN FORMING GIANT PLANET CORES AND PRODUCING HABITABLE CONDITIONS ON TERRESTRIAL PLANETS AND NEUTRAL OXYGEN AT TRACER OF DISK CHEMISTRY AND RADIAL STRUCTURE. HIRMES ALSO MEASURES MOLECULAR HYDROGEN THROUGH ITS TRACER HYDROGEN DEUTERIDE HD WHICH SHOULD MAKE UP MOST OF A PROTOPLANETARY DISK MASS BUT IS NOT ACCESSIBLE WITH EXISTING INSTRUMENTS. HIRMES WITH ITS HIGH SPECTRAL RESOLUTION RESOLVES NARROW EMISSION LINES AND INDEPENDENTLY DETERMINES THEIR ORIGIN IN A DISK FROM VELOCITY INFORMATION THUS BREAKING DEGENERACIES IN COMPLEX DISK MODELS. HIRMES MEASUREMENTS TRACE DISK DENSITY TEMPERATURE AND VELOCITY STRUCTURE AS WELL AS H2O VAPOR AND ICE TO LOCATE THE TRANSITION ZONE BETWEEN GASEOUS AND FROZEN WATER. OBSERVATIONS OF H2 OR BETTER YET ITS DEUTERATED COUNTERPART HD CAN UNIQUELY DETERMINE THE DISK GAS MASS AND THE DEGREE OF SETTLING OF THE SOLID MATERIAL IN DISKS. HIRMES PROVIDES A UNIQUE SPECTROSCOPIC CAPABILITY FOR SOFIA THROUGH ITS HIGH SENSITIVITY TYPICALLY 1 X 10-17 WM-2 OR BETTER AT 5??IN 1 HR 3 KM/S RESOLUTION AND HIGH SPECTRAL RESOLVING POWER R=?/ ???= 105 OVER THE 25 TO 122 M WAVELENGTH RANGE. THIS SPECTRAL REGION CONTAINS LOW-LYING TRANSITIONS OF HD AND H2O AS WELL AS THE STRONG OI 63 M LINE AND A LARGE NUMBER OF OTHER IMPORTANT IONIC ATOMIC AND MOLECULAR LINES FIGURE ES-2. THE INFRARED SPECTROGRAPH IRS ON SPITZER PROVIDED DATA UP TO ~37 M WITH A SPECTRAL RESOLVING POWER OF 600 WHICH IS TWO ORDERS OF MAGNITUDE LESS THAN HIRMES AND INSUFFICIENT TO RESOLVE LINES FROM PROTOPLANETARY DISKS. HIRMES RANGE CONTAINS THE TWO WATER-ICE FEATURES THAT ARE THE ONLY EMISSION TRACERS OF ICE IN PROTOPLANETARY DISKS AND HAVE BEEN POORLY COVERED BY PREVIOUS SPACE MISSIONS. THIS ENSEMBLE OF DIAGNOSTIC TOOLS WHICH WILL BE UNIQUE TO SOFIA WHEN IT INCORPORATES HIRMES PROMISES TO PROVIDE NEW INSIGHT INTO THE EVOLUTION OF PLANETARY SYSTEMS. HIRMES ON SOFIA CONTRIBUTES IN A UNIQUE WAY EVEN IN THE ERA OF ATACAMA LARGE MILLIMETER ARRAY ALMA JAMES WEBB SPACE TELESCOPE JWST HERSCHEL SPITZER AND ALL CURRENT AND PLANNED SOFIA INSTRUMENTS. THE HERSCHEL/PHOTOCONDUCTOR ARRAY CAMERA AND SPECTROMETER PACS PROVIDED SPECTRAL DATA AT WAVELENGTHS>55 M BUT ITS RELATIVELY LOW SPECTRAL RESOLVING POWER IS INSUFFICIENT TO OBTAIN LINE PROFILES FROM GALACTIC SOURCES. THE MID-INFRARED INSTRUMENT MIRI ON JWST WILL OPERATE TO 28 M WITH A SPECTRAL RESOLVING POWER OF 3000 WHICH IS 30 TIMES LESS THAN THAT PROVIDED BY HIRMES. THE SOFIA/ECHELON-CROSS-ECHELLE SPECTROGRAPH EXES AND SOFIA/GERMAN RECEIVER FOR ASTRONOMY AT TERAHERTZ FREQUENCIES GREAT INSTRUMENTS HAVE SMALL WAVELENGTH OVERLAPS WITH HIRMES. EXES AND HIRMES OVERLAP BETWEEN 25 AND 27 M; HOWEVER HIRMES HAS SIGNIFICANTLY HIGHER SENSITIVITY IN THE SPECTRAL OVERLAP REGION.

A 2001 XMM SPECTRUM OF RADIO-LOUD AGN 3C 223 REVEALED THAT THE LINE-OF-SIGHT COLUMN DENSITY IS SIGNIFICANTLY DIFFERENT FROM THE AVERAGE GLOBAL COLUMN DENSITY.

THE PI REQUESTS FUNDS TO ANALYZE AND PUBLISH XMM-NEWTON AO-19 OBSERVATIONS OF SUPER SPIRAL GALAXY 2MFGC 12344. THE FUNDS WILL BE APPLIED TO SALARY BENEFITS AND PAGE CHARGES FOR THE PI AND A GRADUATE STUDENT. DATA ANALYSIS WILL INVOLVE THE REDUCTION OF X-RAY DATA FROM THE EPIC PN AND MOS INSTRUMENTS USING THE XMM SAS AND CUSTOM DATA ANALYSIS SCRIPTS. WITH THIS ANALYSIS WE WILL DETERMINE THE MASS AND PHYSICAL STATE OF THE HALO OF THE FASTEST ROTATING SUPER SPIRAL. THESE PARAMETERS WILL GIVE KEY NEW INSIGHTS INTO THE FORMATION AND EVOLUTION OF THE MOST MASSIVE SPIRAL GALAXIES.

RESEARCH EXPERIENCES FOR UNDERGRADUATE (REU) SITE PROGRAM AT THE NATIONAL SOLAR OBSERVATORY (NSO)

OPTIMIZATION OF THE ROMAN CORONAGRAPH SCIENCE COMMISSIONING AND CALIBRATIONS

SOLAR PHYSICS RELIES HEAVILY ON PROBING THE SUN USING DIAGNOSTICS AVAILABLE ACROSS THE ELECTROMAGNETIC SPECTRUM IN ORDER TO SAMPLE MULTIPLE REGIONS OF THE SOLAR ATMOSPHERE. THE FORMATION MECHANISMS AT DIFFERENT WAVELENGTHS OFFER INSIGHTS INTO A VARIETY OF UNDERLYING PHYSICAL PROCESSES. SPACECRAFT ABOVE THE EARTH'S ATMOSPHERE ARE THE ONLY WAY TO ACCESS THE DIAGNOSTICS IN THE UV AND XRAY OR THEY CAN LEVERAGE THE ADVANTAGE OF CONTINUOUS SEEING-FREE COVERAGE. GROUND-BASED OBSERVATORIES INSTEAD CAN PROBE DIAGNOSTICS IN THE VISIBLE INFRARED AND RADIO WITH GREAT DETAIL AND FLEXIBILITY. PRECISELY COMBINING DATA FROM THESE DIFFERENT OBSERVATORIES HAS PROVED TO BE HIGHLY IMPORTANT TO INCREASING OUR UNDERSTANDING OF THE STRUCTURING AND DYNAMICS OF THE SOLAR ATMOSPHERE. BOTH SPACE- AND GROUND-BASED INSTRUMENTS CONTINUE TO INCREASE THEIR SPATIAL RESOLUTION TO BETTER RESOLVE PHYSICAL PROCESSES AT THEIR FUNDAMENTAL SCALES. THIS HOWEVER INCREASES THE REQUIREMENTS AND COMPLEXITY OF PRECISELY REMAPPING THESE DIFFERENT IMAGES ONTO A COMMON SPATIO-TEMPORAL REFERENCE. SOME OF THESE ISSUES ARE FOUND ACROSS ALL INSTRUMENTS SUCH AS OPTICAL DISTORTIONS OR TIME-VARYING JITTER AND ROLL. OTHER PROBLEMS MIGHT BE MORE SPECIFIC TO GROUND-BASED DATA INCLUDING ATMOSPHERIC REFRACTION TURBULENT IMAGE DISTORTION AND VARIABLE TRANSMISSION. GENERALLY THE COORDINATE DEFINITIONS GIVEN IN THE DATA HEADERS ARE NOT SUFFICIENTLY ACCURATE FOR MANY SCIENTIFIC NEEDS. THEREFORE IT IS NECESSARY TO USE THE DATA THEMSELVES OR OTHER CALIBRATIONS TO ACHIEVE THE CORRECT MAPPING AND GENERATE A PROPERLY ALIGNED DATASET SUITABLE FOR PROPER SCIENTIFIC EXPLOITATION. THIS CURRENTLY REQUIRES EXPERT KNOWLEDGE MANUAL CALIBRATION AND THE USE OF LIMITED-AVAILABILITY CODES WRITTEN IN A PROPRIETARY LANGUAGE. WE PROPOSE TO PRODUCE AN OPEN-SOURCE PROPERLY ENGINEERED TOOLKIT IN PYTHON THAT CAN ADDRESS SOME OF THESE ISSUES AND MAKE IT MORE FEASIBLE FOR THE BROADER COMMUNITY TO SEAMLESSLY COMBINE DATASETS FROM SATELLITES AND GROUND-BASED INSTRUMENTATION. THIS WOULD EMPOWER BROADER USE OF DATA FROM MULTIPLE SOURCES IN A ROBUST FASHION. THIS DEVELOPMENT WOULD USE RELY HEAVILY ON EXISTING PROJECTS SUCH AS SUNPY ASTROPY AND OTHERS TO HANDLE SOME OF THE KEY UNDERLYING TASKS OF DATA RETRIEVAL COORDINATE DEFINITION DATA-CUBE MANIPULATION. THIS TOOLKIT WILL PROVIDE TOOLS TO PERFORM SPECIFIC TASKS SUCH AS NON-RIGID ALIGNMENT BETWEEN IMAGES CORRECTION FOR PLATE-SCALE DISTORTIONS AND COMPENSATION FOR ATMOSPHERIC VARIATIONS. WE PLAN TO WORK WITH THE PYTHON IN HELIOPHYSICS COMMUNITY AND ENSURE THAT THE TOOLKIT WILL BE COMPLIANT WITH THEIR AGREED UPON SOFTWARE STANDARDS. THIS TOOLKIT WILL ALSO BE LEVERAGED IN THE ONGOING DEVELOPMENT OF AN OPEN-SOURCE VISUALIZATION TOOL THAT WILL ALLOW SPACECRAFT AND GROUND-BASED DATA TO BE EASILY VIEWED TOGETHER PROBING ALSO THE TEMPORAL AND SPECTRAL DIMENSIONS OF THE DATACUBES GENERATED BY DIFFERENT INSTRUMENTS. THIS WILL BE APPLIED ESPECIALLY TO DKIST OBSERVATIONS ALLOWING USERS TO JOINTLY EXPLORE THOSE COMPLEX DATA TOGETHER WITH DATA FROM A VARIETY OF NASA ASSETS (SDO IRIS HINODE PSP AND OTHERS). THIS VISUALIZATION TOOL WILL MAKE THE DATA MORE ACCESSIBLE WHILE THE PRECISE CO-ALIGNMENT OF THE DATA FROM VARIOUS SOURCES WILL ALLOW SCIENTIFICALLY IMPORTANT FEATURES TO BE IDENTIFIED MORE EFFICIENTLY. WITH ACCURATE CO-ALIGNMENT AND USER-FRIENDLY DATA MANIPULATION THIS WILL BE A KEY WAY FOR USERS TO IDENTIFY COMBINE AND EXPLORE DATA FROM MULTIPLE OBSERVATORIES.

SCIENCE GOALS AND OBJECTIVES THIS PROPOSED WORK WILL CREATE A SPECIFIC DATA SET FOR STUDYING DEEP MERIDIONAL FLOW PROFILE FROM 30 MM BELOW THE SOLAR SURFACE UP TO TACHOCLINE REGION AND WILL USE HMI/SDO DATA. AN IMPORTANT GOAL OF SOLAR PHYSICS IS THE UNDERSTANDING OF THE MECHANISMS OF SOLAR ACTIVITY AS A PROBLEM IN ITS OWN RIGHT AND FOR ITS IMPORTANCE IN DETERMINING SPACE WEATHER. SOME CLUES TO THE PUZZLE SHOULD ARISE FROM STUDYING THE PHYSICAL PROCESSES IN THE DEEP CONVECTION ZONE SINCE IT IS THE MOTIONS IN THIS REGION THAT ARE THOUGHT TO REGENERATE THE POLOIDAL MAGNETIC FIELD FROM THE TOROIDAL MAGNETIC FIELD AN ESSENTIAL PROCESS THAT ALLOWS THE SOLAR CYCLE TO CONTINUE. WHILE SUBSTANTIAL PROGRESS HAS BEEN ACHIEVED IN UNDERSTANDING SOLAR CONVECTION-ZONE DYNAMICS AND ITS RELATION TO SURFACE ACTIVITY SOME IMPORTANT PROBLEMS STILL REMAIN SUCH AS THE NATURE OF THE DEEP MERIDIONAL FLOW THAT DRIVES THE DYNAMO. RECENT MEASUREMENTS OF EQUATORWARD COMPONENT OF THE MERIDIONAL FLOW FROM HMI AND GONG DATA SHOW SIMILAR PATTERN OF GENERAL PICTURE OF THE FLOW PROFILE. HOWEVER THERE ARE SOME CONTROVERSIAL RESULTS AS WELL. FOR EXAMPLE MULTI-CELL STRUCTURE OF THE MERIDIONAL FLOW (IN DEPTH AND LATITUDE) IS DIFFERENT IN TWO INDEPENDENT MEASUREMENTS. MOST OF THE DISAGREEMENTS MAY BE DUE TO THE FACT THAT THESE MEASUREMENTS ARE NOT FROM STANDARD HMI OR GONG DATA PRODUCT. THEY ARE DERIVED USING DIFFERENT PROCESSING AND MEASUREMENT TECHNIQUES. STANDARD PIPELINES DOES NOT PRODUCE SUCH TYPE OF DATA. MOREOVER DEEP FLOW MEASUREMENTS ARE VERY SENSITIVE TO ANALYSIS METHODS AND PARAMETERS OF DATA PROCESSING E.G. PROJECTION FILTERING ETC. WE PROPOSE TO CREATE VERY UNIQUE AND SPECIALIZED DATA PRODUCTS WHICH WILL CATER TO ALL INTERESTED HELIOPHYSICS COMMUNITY WITH A UNIFORMLY PROCESSED AND WELL ACCEPTED PROCESSING PARAMETERS SINCE STANDARD HMI PIPELINE DOES NOT PRODUCE SUCH TYPE OF DATA. FURTHER PROCESSING OF SUCH DATA SETS IS COMPUTATIONALLY INTENSIVE. THUS AVAILABILITY OF THESE DATA WILL FACILITATE MANY RESEARCH GROUPS TO WORK ON UNIFORM DATA EVEN IF THEY DO NOT HAVE THE PROCESSING CAPABILITIES TO PRODUCE SUCH DATA.

SCIENCE GOALS AND OBJECTIVES: WE PROPOSE TO CREATE A WELL DOCUMENTED CALIBRATED DATASET OF THE HELICITY OF SUBSURFACE FLOWS DERIVED FROM SDO-HMI FOR SCIENTIFIC INVESTIGATIONS BY THE HELIOPHYSICS COMMUNITY. HELICITY PLAYS AN IMPORTANT ROLE IN A BROAD RANGE OF SOLAR PHENOMENA FROM THE DYNAMO TO FLARES AND CORONAL MASS EJECTIONS CMES. HELICITY-LOADED FIELDS ARE VERY PROBABLY RESPONSIBLE FOR THE MOST GEO-EFFECTIVE SOLAR PHENOMENA SUCH AS CMES AND FLARES. EXCESS OF HELICITY IN CORONAL MAGNETIC STRUCTURES CAN LEAD TOTHEIR INSTABILITY AND ERUPTION. THE SIGNATURE OF HELICITY FLOW FROM THE SOLAR INTERIOR TO THE PHOTOSPHERE AND CHROMOSPHERE IS THEREFORE VITAL FOR A BETTER UNDERSTANDING OF THE ROLE OF HELICITY IN SOLAR FLARE-CME ACTIVITY. THE KINETIC HELICITY OF SUBSURFACE FLOWS CAN BE USED AS A PROXY OF MAGNETIC-CURRENT HELICITY IN THE SOLAR INTERIOR AND WILL BE CRUCIAL FOR STUDIES OF THE EVOLUTION OF ACTIVE REGIONS THEIR FLARE ACTIVITY AND THE PROPAGATION OF HELICITY. THE PROPOSED DATA PRODUCT WILL THUS PROVIDE A CRUCIAL LINK BETWEEN THE EVOLUTION OF MAGNETIC FIELDS BELOW THE SURFACE AND THAT OBSERVED IN THE SOLAR ATMOSPHERE USING MAGNETOGRAMS. THIS WILL BE THE FIRST TIME THAT SUCH A DATA SET WILL BE MADE AVAILABLE TO THE COMMUNITY. METHODOLOGY WE WILL PRODUCE THREE DATA PRODUCTS: THE KINETIC HELICITY ITS VERTICAL CONTRIBUTION AND THE NORMALIZED HELICITY GRADIENT VARIANCE NHGV PARAMETER THAT CAPTURES THE VARIATION OF KINETIC HELICITY WITH DEPTH AND TIME. THE INPUT MEASUREMENTS ARE THE DAILY SUBSURFACE FLOWS FROM THE SURFACE TO A DEPTH OF 16 MM DERIVED FROM SDO-HMI DOPPLERGRAMS USING THE DRMS RING-DIAGRAM PIPELINE. FROM THESE MEASUREMENTS WE WILL CALCULATE THE PROPOSEDDATA PRODUCTS AS A FUNCTION OF DISK POSITION COVERING THE WHOLE SUN INCLUDING ACTIVE AS WELL AS QUIET REGIONS. THE SUBSURFACE HELICITY OF QUIET REGIONS PROVIDES A SOLAR BACKGROUND AND WILL BE USED TO CALIBRATE THE HELICITY OF ACTIVE REGIONS. THE CADENCE AND THE SPATIAL GRID OF THE FULL-DISK MAPS WILL BE GIVEN BY THOSE OF THE INPUT DATA. WE WILL REMOVE ANY SYSTEMATIC EFFECTS PRESENT IN THE SUBSURFACE FLOW MEASUREMENTS BEFORE CALIBRATING THE HELICITY DATA PRODUCTS. WE HAVE ALREADY TESTED OUR METHOD DERIVING THE HELICITY QUANTITIES FROM EXISTING SUBSURFACE FLOW DATA. WORK PLAN: WE WILL CREATE THE DATA PRODUCTS FROM EXISTING ARCHIVED SUBSURFACE FLOW DATA INCLUDING THEIR CALIBRATION AND DOCUMENTATION. WE WILL CONTINUE TO CREATE NEW DATA PRODUCTS AS SOON AS SUBSURFACE FLOW MEASUREMENTS BECOME AVAILABLE WHICH OCCURS TYPICALLY WITHIN A FEW DAYS FROM SDO-HMI VIA JSOC AND WILL ADD THEM TO THE DATA SET. IN THIS WAY WE WILL CREATE A DATASET THAT CAN BE USED FOR STATISTICAL STUDIES WITH LARGE SAMPLES AS WELL AS FOR AN ANALYSIS OF ACTIVE REGIONS THAT ARE STILL PRESENT ON THE SUN. WE WILL MAKE THE DATA PRODUCTS FITS AND ASCII FILES AVAILABLE IN THE PUBLIC DOMAIN THROUGH WEBSITE ARCHIVESAND VIRTUAL OBSERVATORIES WITH THE HELP OF SOFTWARE ENGINEERS BASED AT NSO. RELEVANCE: MAKING THE SUBSURFACE HELICITY AVAILABLE AS A DATA RESOURCE TO THE HELIOPHYSICS COMMUNITY WILL GREATLY ENHANCE THE SCIENTIFIC RETURN FROM SDO-HMI AND WILL BE CRUCIAL FOR UNDERSTANDING MAGNETIC ACTIVITY FROM THE INTERIOR THROUGH THE SOLAR ATMOSPHERE. THIS PROPOSAL THUS ADDRESSES NASA STRATEGIC SUBGOAL 2.2: UNDERSTAND THE SUN AND ITS INTERACTIONS WITH EARTH AND THE SOLAR SYSTEM.

SCIENCE GOALS AND OBJECTIVES: WE PROPOSE TO CREATE A DATASET OF THE (CORRECTED) MERIDIONAL FLOW IN SUB-PHOTOSPHERIC LAYERS (DERIVED MAINLY FROM SDO/HMI) FOR SCIENTIFIC INVESTIGATIONS BY THE HELIOPHYSICS COMMUNITY. THE MERIDIONAL FLOW PLAYS AN IMPORTANT ROLE IN A BROAD RANGE OF SOLAR PHENOMENA FROM THE DYNAMO TO THE EVOLUTION OF POLAR MAGNETIC FIELDS AND THE PREDICTION OF THE SOLAR CYCLE. THE LATITUDINAL PROFILE OF THE MERIDIONAL FLOW IS A KEY INGREDIENT IN SURFACE FLUX-TRANSPORT MODELS AND GREATLY INFLUENCES THE POLAR FIELD EVOLUTION. THE MERIDIONAL FLOW IS THUS A CRUCIAL COMPONENT OF THE EVOLUTION OF SURFACE MAGNETIC FLUX. THE STRUCTURE AND THE STRENGTH OF THE MERIDIONAL FLOW SETS THE TIMING OF THE SOLAR CYCLE IN FLUX-TRANSPORT DYNAMO MODELS. THE MERIDIONAL FLOW AND ITS TEMPORAL VARIATION ARE THUS A CRUCIAL PART IN PREDICTING THE SOLAR CYCLE. WITH ITS COMPARABLY SMALL AMPLITUDE (ABOUT TWO ORDERS OF MAGNITUDE SMALLER THAN THE SOLAR ROTATION RATE) THE MERIDIONAL FLOW IS SUSCEPTIBLE TO SYSTEMATICS AND ROBUST MEASUREMENTS ARE NOT EASILY AVAILABLE. WE PROPOSE TO CREATE A DATA PRODUCT THAT IS CORRECTED FOR SYSTEMATICS AND IS CONSISTENT DURING DIFFERENT PHASES OF THE SOLAR CYCLE. THE PROPOSED DATA PRODUCT CAN THUS BE USED AS INPUT DATA IN MODELING EFFORTS OR AS A BENCHMARK TO COMPARE MODEL PREDICTIONS AGAINST. MAKING THE CORRECTED SUBSURFACE MERIDIONAL FLOW AVAILABLE AS A DATA RESOURCE TO THE HELIOPHYSICS COMMUNITY WILL GREATLY ENHANCE THE SCIENTIFIC RETURN FROM SDO/HMI AND WILL BE CRUCIAL FOR UNDERSTANDING THE POLEWARD TRANSPORT OF MAGNETIC ACTIVITY AND PREDICTING THE SOLAR CYCLE. METHODOLOGY: WE WILL PRODUCE THE FOLLOWING DATA PRODUCT: THE MERIDIONAL FLOW AT SEVERAL DEPTHS IN THE SUBSURFACE LAYERS AS A FUNCTION OF LATITUDE AND TIME. THE INPUT MEASUREMENTS ARE THE SUBSURFACE FLOWS DERIVED FROM SDO/HMI DOPPLERGRAMS ANALYZED WITH THE RING-DIAGRAM TECHNIQUE FROM THE SURFACE TO A DEPTH OF 16 MM. FROM THE DAILY FULL-DISK FLOW MAPS (INPUT DATA) WE WILL CALCULATE THE AVERAGE MERIDIONAL FLOW (PROPOSED DATA PRODUCT) AVERAGED OVER EACH COMPLETE CARRINGTON ROTATION. WE WILL REMOVE SYSTEMATIC EFFECTS PRESENT IN THE SUBSURFACE FLOW MEASUREMENTS SUCH AS SYSTEMATIC VARIATIONS WITH DISK POSITION AND ANNUAL VARIATIONS DUE TO THE B0 AND P ANGLE AND AVERAGE THE CORRECTED FLOWS OVER EACH CARRINGTON ROTATION. THEN WE WILL USE SOHO/MDI AND GONG DATA TO GENERATE THE CORRECTED MERIDIONAL FLOW FOR SOLAR CYCLE 23 IN ADDITION TO CYCLE 24 COVERED BY SDO/HMI DATA. WE HAVE ALREADY TESTED OUR METHOD ON EXISTING (ARCHIVED) SUBSURFACE FLOW DATA AND PLAN TO CREATE THESE DATASETS FIRST INCLUDING THEIR CALIBRATION AND DOCUMENTATION. WE WILL THEN CREATE NEW DATA PRODUCTS AS SOON AS A FULL CARRINGTON ROTATIONS OF SUBSURFACE FLOW MEASUREMENTS BECOME AVAILABLE FROM SDO/HMI (VIA JSOC) AND WILL ADD THEM TO THE DATA SET. IN THIS WAY WE WILL CREATE A DATASET THAT CAN BE USED FOR STUDIES OF THE SOLAR CYCLE AS WELL AS FOR MODELING LATITUDINAL FLUX TRANSPORT OF THE CURRENT SUN.

SUBSURFACE ZONAL AND MERIDIONAL FLOW FROM BIG RINGS: A DATASET FOR STUDYING THE LONG-TERM EVOLUTION OF MAGNETIC FLUX AND THE DYNAMICS OF THE CONVECTION ZONE

SCIENCE GOALS THIS PROPOSAL WILL ENABLE: FULL DISK PHOTOSPHERIC MAGNETOGRAMS ARE ONE OF THE MOST IMPORTANT DATASETS OF MODERN RESEARCH IN SOLAR PHYSICS. THE MAGNETOGRAMS ARE INVALUABLE FOR UNDERSTANDING AND MODELING OF PRACTICALLY ALL SOLAR PHENOMENA INCLUDING SOLAR CYCLE CORONA SOLAR ERUPTIVE ACTIVITY HELIOSPHERE AND SPACE WEATHER. TWO MAJOR LIMITATIONS OF HISTORICAL MAGNETOGRAPH DATA WHICH ARE CURRENTLY IN PUBLIC DOMAIN INCLUDE (1) THEIR LIMITED TIME COVERAGE (MID-1970-PRESENT) AND (2) POSSIBLE UNCERTAINTIES IN CALIBRATION OF MAGNETIC FIELDS OF EARLY MAGNETOGRAMS WHICH COULD BE ALLEVIATED VIA COMPARISON WITH MULTIPLE INSTRUMENTS.

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