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Discoveries of terrestrial, Earth-sized exoplanets that lie within thehabitable zone (HZ) of their host stars continue to occur at increasing rates.Transit spectroscopy can potentially enable the detection of molecularsignatures from such worlds, providing an indication of the presence of anatmosphere and its chemical composition, including gases potentially indicativeof a biosphere. Such planets around nearby M-dwarf stars - such as TRAPPIST-1 -provide relatively good signal, high signal/noise, and frequent transits forfollow-up spectroscopy. However, even with these advantages, transitspectroscopy of terrestrial planets in the HZ of nearby M-stars will still be achallenge. Herein, we examine the potential for future space observatories toconduct such observations, using a Global Climate Model (GCM), a photochemicalmodel, and a radiative transfer suite to simulate modern-Earth-like atmosphericboundary conditions on TRAPPIST-1e. The detectability of biosignatures on suchan atmosphere via transmission spectroscopy is modeled for JWST, LUVOIR, HabEx,and Origins. We show that for any of these observatories, only CO2 would bedetectable at the 3 sigma level in transmission spectroscopy, when clouds areincluded in our simulations. This is because the impacts of clouds on scaleheight strongly limits the detectability of molecules in the atmosphere.Synergies between space- and ground-based spectroscopy may be essential inorder to overcome these difficulties.

Detectability of Molecular Signatures on TRAPPIST-1e through Transmission Spectroscopy Simulated for Future Space-Based Observatories