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.