THIS PROPOSED WORK WILL ENABLE THE SUCCESSFUL INTERPRETATION OF ATMOSPHERIC EXOPLANET DATA FOR ALL CURRENT AND FUTURE NASA MISSIONS. IN PARTICULAR FUTURE NASA MISSIONS SUCH AS JWST IN COMPARISON TO HST AND SPITZER WILL HAVE BROADER WAVELENGTH COVERAGE AND SPECTRAL RESOLUTION ENABLING THE DETECTION OF A VARIETY OF MOLECULAR FEATURES AT HIGH SNR. THESE NEW DISCOVERIES WILL BRING FORTH INSIGHTS INTO PLANETARY ATMOSPHERIC PHYSICS AND CHEMISTRY THROUGH OUR ABILITY TO MEASURE ROBUST ATMOSPHERIC ABUNDANCES. FOR EXAMPLE THE CANONICAL TECHNIQUES TO ADDRESS QUESTIONS OF PLANET FORMATION INCLUDE MEASURING CARBON-TO-OXYGEN RATIOS IN PLANETARY ATMOSPHERES TO INFER WHERE THE PLANET FORMED IN THE PROTOPLANETARY DISK AND MEASURING METAL ABUNDANCES OF PLANET ATMOSPHERES IN ORDER TO COMPARE WITH THE HOST STAR METALLICITY. FURTHERMORE INTERPRETING THE HABITABILITY OF TEMPERATE TERRESTRIAL WORLDS WILL ALSO REQUIRE AN ANALYSIS OF THE CHEMICAL MAKEUP OF THE ATMOSPHERE. ESSENTIALLY ALL OBSERVATIONS OF EXOPLANET ATMOSPHERES WITH FUTURE NASA MISSIONS WILL REQUIRE MEASURING THE ABUNDANCES OF KEY MOLECULES SUCH AS H2O CO CH4 OR CO2. BECAUSE ROBUST OPACITIES ARE REQUIRED AS INPUT TO NEARLY ALL SPECTROSCOPIC MODELS THAT WILL BE USED TO INTERPRET EXOPLANET ATMOSPHERE DATA FROM FUTURE MISSIONS THIS PROGRAM IS DIRECTLY RELEVANT TO NASA OBJECTIVES TO ROBUSTLY CHARACTERIZE EXTRASOLAR PLANETS.