THIS STUDY FOCUSES ON PRECISE MEASUREMENTS OF THE DEEP MERIDIONAL FLOW AND ITS TEMPORAL VARIATIONS FROM THE SOLAR SURFACE DOWN TO THE BOTTOM OF THE SOLAR CONVECTIVE ZONE. MERIDIONAL CIRCULATION IS AN IMPORTANT COMPONENT OF ALL DYNAMO MODELS AS ITS STRENGTH DETERMINES KEY CHARACTERISTICS OF THE SOLAR ACTIVITY CYCLE. FOR MORE THAN 20 YEARS THE MERIDIONAL FLOW HAS BEEN MEASURED BY DIFFERENT TECHNIQUES AS A FLOW TOWARDS THE POLES IN BOTH HEMISPHERES NEAR THE SURFACE. AS MASS IS NOT ACCUMULATING AT THE POLES THERE MUST BE AN EQUATORWARD RETURN FLOW SOMEWHERE DEEPER IN THE CONVECTIVE ZONE WHICH HAS NOT BEEN CONSISTENTLY OBSERVED FROM HELIOSEISMIC MEASUREMENTS. TRADITIONAL TIME-DISTANCE MEASUREMENTS OF THE MERIDIONAL FLOW ARE BASED ON OBTAINING ACOUSTIC TRAVEL TIME DIFFERENCES BETWEEN OPPOSITELY PROPAGATING WAVES IN THE NORTH-SOUTH DIRECTIONS. THESE TIME DIFFERENCES ARE A PRODUCT OF THE SUPERPOSITION OF BOTH THE SURFACE POLEWARD AND THE DEEP EQUATORWARD MERIDIONAL CIRCULATION. SINCE THE POLEWARD COMPONENT IS MUCH LARGER THAN THE RETURN COMPONENT (BY A FACTOR OF 5-10) SUBSTANTIAL AVERAGING IS NEEDED TO EXTRACT THE WEAKER RETURN FLOW. CROSS-CORRELATIONS BETWEEN TWO LOCATIONS SEPARATED BY LARGE ENOUGH DISTANCES (THE RAYPATH CONNECTING THESE TWO LOCATIONS IS VERTICAL NEAR THE SURFACE AND THE SENSITIVITY TO THE SURFACE HORIZONTAL POLEWARD FLOW IS MINIMAL) SHOULD BE MOST SENSITIVE ONLY TO THE RETURN EQUATORWARD FLOWS. A RECENT APPROACH FOR REMOVING AN IMPORTANT OBSERVED SYSTEMATIC CENTER-TO-LIMB VARIATIONS IN TIME-DISTANCE MEASUREMENTS (ZHAO ET AL. 2012) OPENS UP NEW POSSIBILITIES FOR LOOKING AT DEEP FLOW PROFILES AND WE ESTIMATE THAT THE DEEP EQUATORWARD FLOW CAN BE RECOVERED BY USING 2-3 YEARS OF OBSERVATIONS (KHOLIKOV AND HILL 2014). SIMILAR ANALYSIS FROM TWO INDEPENDENT HMI AND GONG DATA MADE IT POSSIBLE TO DETECT A SOMEWHAT UNEXPECTED SHALLOW RETURN MERIDIONAL (ZHAO ET AL. 2013 KHOLIKOV ET AL. 2014 JACKIEWICZ ET AL. 2015) AT ABOUT 0.9R. DESPITE THE FACT THAT THE DATA AND PROCESSING PROCEDURES WERE COMPLETELY DIFFERENT THE FLOW PROPERTIES IN THE UPPER HALF OF THE CONVECTION ZONE ARE IN VERY GOOD AGREEMENT. HOWEVER THE DEEPEST CONVECTIVE LAYERS REMAIN HIGHLY UNCERTAIN. IN THIS PROPOSED WORK WE WILL MAKE SEVERAL IMPORTANT IMPROVEMENTS. FIRST WE WILL EXTEND OUR ANALYSIS TO ALL AVAILABLE HMI DATA. THUS WE CAN IMPROVE THE STATISTICAL SIGNIFICANCE OF OBTAINED MERIDIONAL FLOW PARAMETERS THAT CAN THEN BE USED IN SOLAR DYNAMO MODELS. SECOND WE WILL USE A NEWLY PRODUCED DATA SET OF SPHERICAL HARMONIC COEFFICIENTS THAT USE A WIDER APODIZATION OF THE HMI VELOCITY IMAGES TO 75 DEGREES (THE PREVIOUS HMI AND GONG DATA WERE LIMITED TO ABOUT 66 DEGREES) WHICH WILL ALLOW US TO MAKE LARGER DISTANCE MEASUREMENTS AND USE BETTER AVERAGING. FINALLY OUR INVERSIONS WILL USE NEWLY COMPUTED BORN-APPROXIMATION SENSITIVITY KERNELS IN SPHERICAL GEOMETRY (BOENING ET AL. 2017) PROVIDED BY ONE OF OUR TEAM MEMBERS. THESE KERNELS ARE COMPUTED PRECISELY FOR INVERTING MEASUREMENTS SUCH AS THESE AND CAN ALSO BE USED IN INVERSIONS TO HELP DISCERN SMALLER-SCALE FLOW FEATURES AND VARIATIONS THAN TRADITIONAL RAY KERNELS (USED IN ALL STUDIES TO DATE) CAN SENSE. IN ADDITION TO THE DETAILED FLOW PROFILE WE WILL BE ABLE TO INVESTIGATE TEMPORAL VARIATIONS OF THE RETURN MERIDIONAL FLOW BY PRODUCING SEVERAL INDEPENDENT MEASUREMENTS DURING 2010 2017 TIME PERIOD. WE WILL USE THE HMI HIGH-RESOLUTION MEASUREMENTS TO INVESTIGATE HIGH LATITUDE REGIONS (GREATER THAN 60 DEGREES) WHERE THE POLEWARD FLOW MAY CHANGE ITS DIRECTION AS HAS BEEN OBSERVED IN SEVERAL PAST STUDIES HOWEVER WITH SOME SIGNIFICANT UNCERTAINTY. THE PROPOSED WORK PARTIALLY ADDRESSES SEVERAL SCIENCE GOALS FROM THE RECENT HELIOPHYSICS DECADAL SURVEY: (1) DETERMINE THE ORIGINS OF THE SUN'S ACTIVITY AND PREDICT THE VARIATIONS IN THE SPACE ENVIRONMENT; (2) DISCOVER AND CHARACTERIZE FUNDAMENTAL PROCESSES THAT OCCUR BOTH WITHIN THE HELIOSPHERE AND THROUGHOUT THE UNIVERSE.