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Atmospheric spectroscopy of an exciting array of exoplanets (warm rocky planets sub-Neptune and Jupiter mass planets) will be obtained during JWST.s Cycle 1. To accurately model and interpret observations of these planets. atmospheres we must understand the high-energy SED of their host stars: FUV and NUV-driven photochemistry shapes an atmosphere.s molecular abundances and the formation of hazes EUV irradiation can erode a planet.s gaseous envelope and flares can affect long term atmospheric stability. [truncated! Please see actual data for full text]