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Characterizing rocky exoplanet atmospheres is a key goal of exoplanetscience, but interpreting such observations will require understanding thestellar UV irradiation incident on the planet from its host star. Stellar UVmediates atmospheric escape, photochemistry, and planetary habitability, andobservations of rocky exoplanets can only be understood in the context of theUV SED of their host stars. Particularly important are SEDs fromobservationally favorable but poorly understood low-mass M-dwarf stars, whichare the only plausible targets for rocky planet atmospheric characterizationfor the next 1-2 decades. In this work, we explore the utility of AstroSat UVITfor the characterization of the UV SEDs of low-mass stars. We presentobservations of the nearby M0 star HIP 23309 in the FUV and NUV gratings ofUVIT. Our FUV spectra are consistent with contemporaneous HST data and our NUVspectra are stable between orbits, suggesting UVIT is a viable tool for thecharacterization of the SEDs of low-mass stars. We apply our measured spectrato simulations of photochemistry and habitability for a hypothetical rockyplanet orbiting HIP 23309 and elucidate the utility and limitations of UVIT inderiving UV SEDs of M-dwarf exoplanet hosts. Our work validates UVIT as a toolto complement HST in the characterization of exoplanet host stars and carriesimplications for its successor missions like INSIST.

UV Spectral Characterization of Low-Mass Stars With AstroSat UVIT for Exoplanet Applications: The Case Study of HIP 23309