UNDERSTANDING GALAXY FORMATION AND EVOLUTION AND THE PHYSICAL PROCESSES THAT DRIVE THEM IS ONE OF THE MOST IMPORTANT CHALLENGES OF PHYSICAL COSMOLOGY AND A CENTRAL DRIVER OF GROUND- AND SPACE-BASED OBSERVING PROGRAMS. THE CIRCUMGALACTIC MEDIUM (CGM) AND INTERGALACTIC MEDIUM (IGM) ARE INTERCONNECTED REPOSITORIES FOR BARYONS WHICH MOVE FROM THE IGM THROUGH THE CGM AND THEN ONTO GALAXIES THROUGH BOTH HOT AND COLD MODES OF ACCRETION. SOME OF THESE BARYONS FORM STARS AND CENTRAL BLACK HOLES BUT MOST LEAVE GALAXIES THROUGH SUPERNOVA AND QUASAR WINDS AND REJOIN THE CGM FROM WHICH THEY CAN POTENTIALLY REACCRETE. MOST OF THE EVIDENCE FOR THIS BARYON CYCLE PARADIGM IS INDIRECT ARISING FROM THE STUDY OF GALAXY STELLAR MASSES METALLICITIES AND STAR FORMATION RATES OVER COSMIC TIME. TO STUDY THIS PARADIGM DIRECTLY ONE MUST FOCUS ON THE CGM WHICH IS GROUND ZERO FOR THESE PROCESSES. SPACE-BASED UV ABSORPTION-LINE SPECTROSCOPY IS THE MOST POWERFUL TOOL FOR STUDYING THIS MEDIUM PROVIDING INFORMATION ON MASS AND METAL CONTENT AND PHYSICAL CONDITIONS. YET INTERPRETING THESE OBSERVATIONS REQUIRES DETAILED MODELING OF INTERACTIONS AT WIND/HALO GAS INTERFACES THAT OCCUR ON SCALES MUCH BELOW THE RESOLUTION OF ANY CURRENT GALAXY FORMATION SIMULATION. TO RESOLVE THIS IMPASSE WE WILL IMPLEMENT A NEW WIND ALGORITHM THAT EXPLICITLY MODELS THE SUBGRID PHYSICS IN THE WIND-HALO GAS INTERACTION ANALYTICALLY USING THE SIMULATION TO PROVIDE THE PHYSICAL CHARACTERISTICS THAT INFORM THE INTERACTION. THIS INTRODUCES FREE PARAMETERS BUT WE CAN RESTRICT THEM BY MATCHING VERY HIGH RESOLUTION SIMULATIONS OF INDIVIDUAL CLOUD-CGM INTERACTIONS. OUR EXISTING SIMULATIONS ALREADY REPRODUCE MANY OBSERVED PROPERTIES OF GALAXIES AND METAL-LINE ABSORPTION BUT THE NEW WIND IMPLEMENTATION WILL ALLOW US TO TIE EMPIRICAL SUCCESSES AND FAILURES TO THE UNDERLYING WIND EJECTION MECHANISMS AND THE INTERACTION BETWEEN THE WIND AND THE GASEOUS HALO. THIS WILL ALLOW US FOR THE FIRST TIME TO IDENTIFY ABSORPTION-LINE FEATURES WITH SPECIFIC PHYSICAL PROCESSES. WITH THIS TOOL WE WILL PERFORM LARGE-VOLUME HIGH-RESOLUTION SIMULATIONS THAT WILL HAVE 3E9 PARTICLES IN VOLUMES THAT RANGE FROM 12.5 TO 200 MPC/H ON A SIDE. THESE SIMULATIONS WILL USE A NEW LAGRANGIAN MESHLESS HYDRODYNAMICS CODE GIZMO. SELECTED GALAXIES FROM THESE RUNS WILL BE EVOLVED TO Z=0 USING "ZOOMED" SIMULATIONS OF SUBVOLUMES TO STUDY LOW REDSHIFT EVOLUTION AND CIRCUMGALACTIC GAS ABSORPTION AT VERY HIGH RESOLUTION. IN ADDITION TO MILKY WAY LIKE GALAXIES THE ZOOMED SIMULATIONS WILL TARGET THE CRUCIAL HALO MASS RANGE 1E12-1E13 MSUN WHERE QUASI-STATIC HOT GAS HALOS DEVELOP AND STAR FORMATION IN CENTRAL GALAXIES IS SUPPRESSED. THE SIMULATIONS WILL ALLOW DETAILED TRACKING OF THE MANY MODES OF GALAXY GROWTH IN PARTICULAR THE RELATIVE CONTRIBUTIONS OF COLD FILAMENTARY ACCRETION HOT QUASI-SPHERICAL ACCRETION AND THE RECYCLING OF METAL-ENRICHED WINDS. THESE PREDICTIONS WILL BE TESTED AGAINST A WIDE RANGE OF OBSERVATIONAL DATA INCLUDING: (1) HST AND GROUND-BASED STUDIES OF CIRCUMGALACTIC GAS ABSORPTION (2) GROUND AND SPACE-BASED MEASUREMENTS OF THE EVOLUTION OF GALAXY STELLAR MASSES STAR FORMATION RATES METALLICITIES MORPHOLOGIES AND SPATIALLY RESOLVED KINEMATICS AND CHEMISTRY AND (3) X-RAY OBSERVATIONS OF MASSIVE GALAXIES AND POOR GROUPS. THESE COMPARISONS WILL PLACE TIGHT CONSTRAINTS ON THE PHENOMENOLOGY AND UNDERLYING PHYSICS OF GALACTIC FEEDBACK AND ON THE INTERACTIONS BETWEEN WINDS AND GASEOUS HALOS. THE SUCCESSES AND FAILURES OF THE SIMULATIONS IN REPRODUCING OBSERVATIONS WILL TEST KEY ASPECTS OF THE PHYSICS OF GALAXY FORMATION AND THE INTERACTION BETWEEN GALACTIC WINDS AND THE CGM. TOGETHER THESE STUDIES WILL PROVIDE A COMPREHENSIVE EVOLUTIONARY PICTURE THAT UNIFIES OBSERVATIONS ACROSS A WIDE SPAN OF REDSHIFT WAVELENGTH AND SPATIAL SCALES.