AFTER LIGHT-CURVE CALIBRATION USING THE PHILLIPS RELATION THE DISTANCE TO AN INDIVIDUAL TYPE IA SUPERNOVA (SN IA) CAN BE INFERRED WITH ~5% PRECISION. DISTANCE MEASUREMENTS ENABLE TYPE IA SUPERNOVAE (SNE IA) THE HIGHLY LUMINOUS EXPLOSIONS OF WHITE DWARF STARS TO BE USED AS POWERFUL TOOLS TO ADDRESS TWO OPEN QUESTIONS: (1) IS THE LOCAL VALUE OF THE HUBBLE CONSTANT DIFFERENT FROM THAT INFERRED FROM THE COSMIC MICROWAVE BACKGROUND (CMB)? AND (2) WHAT IS THE NATURE OF THE DARK ENERGY RESPONSIBLE FOR THE ACCELERATING COSMIC EXPANSION? NEARBY SNE IA YIELD A LOCAL VALUE OF THE HUBBLE CONSTANT (74.03 +- 1.42 KM / S / MPC SH0ES TEAM) THAT IS IN STRONG TENSION (~4.4 SIGMA) WITH THAT INFERRED FROM THE CMB (67.4 +- 0.6 KM / S / MPC PLANCK COLLABORATION). IF THE TENSION REPRESENTS A TRUE DIFFERENCE RECONCILING THE INFERRED VALUES MAY REQUIRE NEW PHENOMENA SUCH AS AN ADDITIONAL RELATIVISTIC SPECIES WHICH COULD CAUSE MORE RAPID EXPANSION DURING THE RADIATION-DOMINATED EPOCH. A MISMATCH HOWEVER BETWEEN THE HOST-GALAXY PROPERTIES OF SNE IA IN THE CEPHEID CALIBRATION AND HUBBLE-FLOW SNE SAMPLES USED BY THE SH0ES TEAM COULD RESOLVE THE TENSION. THE SH0ES TEAM CALIBRATES THE ABSOLUTE LUMINOSITIES OF SNE IA USING MASSIVE CEPHEID VARIABLE STARS FOUND ONLY IN STAR-FORMING GALAXIES. THE VALUE OF H0 HOWEVER IS MEASURED USING MORE DISTANT SNE IA FOUND IN BOTH STAR-FORMING AND PASSIVE GALAXIES. WE HAVE KNOWN FOR A DECADE FROM MULTIPLE INDEPENDENT SN SAMPLES THAT SNE IA LUMINOSITIES AFTER CALIBRATION BY LIGHT-CURVE SHAPE AND COLOR SHOW A STRONG ~0.05-0.1 MAGNITUDE DEPENDENCE ON THE STELLAR MASS OF THEIR HOST GALAXIES. THE PHYSICAL ORIGIN OF THIS EFFECT REMAINS POORLY UNDERSTOOD ALTHOUGH IT MAY BE CONNECTED TO PROGENITOR AGE OR METALLICITY OR THE PROPERTIES OF THE DUST. IF CONNECTED TO PROGENITOR AGE THEN THE CURRENT SN IA MEASUREMENT OF H0 BY THE SH0ES TEAM MAY BE SUBSTANTIALLY BIASED. TO EXPLORE WHETHER THE HOST-ENVIRONMENT BIAS IS LINKED TO PROGENITOR AGE A PAIR OF EFFORTS HAVE MEASURED STAR-FORMATION RATES IN THE LOCAL ENVIRONMENTS OF NEARBY SNE IA. HOWEVER THESE EITHER LACK ANY CORRECTION FOR DUST EXTINCTION OR RELY ON STRONG PRIORS. WE PROPOSE TO COMBINE ARCHIVAL UV-THROUGH-IR IMAGING FROM GALEX SDSS PANSTARRS 2MASS AND WISE WITH ALREADY ACQUIRED INTEGRAL-FIELD UNIT (IFU) OPTICAL SPECTRA OF THE HOST GALAXIES OF 94 SNE IA IN THE HUBBLE FLOW. WE WILL ALSO ACQUIRE IFU SPECTRA OF THE CEPHEID HOST GALAXIES USED BY THE SH0ES TEAM. MODELING THESE DATA WITH POPULATION SYNTHESIS MODELS WILL PROVIDE SIGNIFICANTLY IMPROVED MEASUREMENTS ON THE STAR-FORMATION HISTORY METALLICITY AND DUST CONTENT OF THE ENVIRONMENTS OF SNE AND THIS EFFORT WILL PROVIDE MUCH MORE PRECISE MEASUREMENT OF THE ENVIRONMENT-DEPENDENT SN IA CALIBRATION BIAS. MOREOVER WE PROPOSE TO CONSTRUCT SAMPLES OF CEPHEID AND HUBBLE-FLOW SNE WITH MATCHING LOCAL EXPLOSION ENVIRONMENT PROPERTIES THAT WILL YIELD THE FIRST ESTIMATE OF H0 WITHOUT HOST-GALAXY BIAS. IN THE NEXT DECADE THE COMMUNITY WILL INVEST ENORMOUS RESOURCES IN OBSERVING SNE IA WITH THE NANCY GRACE ROMAN SPACE TELESCOPE TO PROBE THE NATURE OF THE DARK ENERGY. THE ROMAN SPACE TELESCOPE WILL TEST DARK-ENERGY MODELS BY COMPARING THE LUMINOSITY DISTANCES OF NEARBY LOW-REDSHIFT SNE WITH THOSE OF A HIGH-REDSHIFT SAMPLE WHOSE HOST GALAXIES ARE COMPARATIVELY METAL POOR AND YOUNG. CORRECTING HOST-DEPENDENT BIAS WILL NOT BE POSSIBLE USING HOST-GALAXY STELLAR MASS GIVEN THE 10 GYRS OF COSMIC EVOLUTION ACROSS THE SAMPLE. INSTEAD A MORE DETAILED MODEL FOR THE VARIATION OF CALIBRATED SN IA LUMINOSITIES IS REQUIRED FOR INFERENCES FROM ROMAN SPACE TELESCOPE SN IA OBSERVATIONS. OUR STUDY OF THE LOCAL ENVIRONMENTS OF LOW-REDSHIFT SNE IA WILL YIELD POSTERIOR DISTRIBUTIONS FOR STELLAR POPULATION AGE AND METALLICITY AND DUST PROPERTIES. THESE WILL ENABLE US TO DEVELOP THE FIRST MODEL IN TERMS OF THESE PHYSICAL PROPERTIES WHICH WILL BE NEEDED TO CORRECT ROMAN SPACE TELESCOPE SN IA MEASUREMENTS.