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TRAPPIST-1e is a potentially habitable terrestrial exoplanet orbiting anultra-cool M Dwarf star and is a key target for observations with the JamesWebb Space Telescope (JWST). One-dimensional photochemical modelling ofterrestrial planetary atmospheres has shown the importance of the incomingstellar UV flux in modulating the concentration of chemical species, such asO$_3$ and H$_2$O. In addition, three-dimensional (3D) modelling hasdemonstrated anisotropy in chemical abundances due to transport in tidallylocked exoplanet simulations. We use the Whole Atmosphere Community ClimateModel Version 6 (WACCM6), a 3D Earth System Model, to investigate howuncertainties in the incident UV flux, combined with transport, affectobservational predictions for TRAPPIST-1e (assuming an initial Earth-likeatmospheric composition). We use two semi-empirical stellar spectra forTRAPPIST-1 from the literature. The UV flux ratio between them can be as largeas a factor of 5000 in some wavelength bins. Consequently, thephotochemically-produced total O$_3$ columns differ by a factor of 26. Spectralfeatures of O$_3$ in both transmission and emission spectra vary between thesesimulations (e.g. differences of 19 km in transmission spectra effectivealtitude for O$_3$ at 0.6 $\mu$m). This leads to potential ambiguities wheninterpreting observations, including overlap with scenarios that assumealternative O$_2$ concentrations. Hence, to achieve robust interpretations ofterrestrial exoplanetary spectra, characterisation of the UV spectra of theirhost stars is critical. In the absence of such stellar measurements,atmospheric context can still be gained from other spectral features (e.g.H$_2$O), or by comparing direct imaging and transmission spectra inconjunction.

Degenerate interpretations of O$_3$ spectral features in exoplanet  atmosphere observations due to stellar UV uncertainties: a 3D case study with  TRAPPIST-1e