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tokens: pCO 2 case for a single multi-epoch case. 1 σ and 2 σ contours are included. 5. Atmospheric Retrievals To perform our retrievals we use the open-source radiative transfer and retrieval framework CHIMERA (Line Yung 2013 ; Line et al. 2013 ). It previously has been used to study the atmosphere of TRAPPIST-1e to determine the resolution that a future instrument needs to have in order to detect and constrain the abundances of molecules in the atmospheres of temperate terrestrial planets to high precision (Tremblay et al. 2020 ). Our retrieval setup is similar to that presented in Tremblay et al. ( 2020 ). For each of the combined spectra we fit for six parameters: an isothermal temperature profile ( T iso ), a radius scaling factor (x R p ), the cloud top pressure (), the mean molecular weight of the atmosphere, and the volume mixing ratio of H 2 O and CO 2 . We use the mean molecular weight (MMW) as a proxy to effectively fill the rest of the atmosphere with N 2 as this molecule is inert. 6. Results Each spectra that we retrieved had a different underlying cloud configuration, hence we wanted to determine if these physical processes impact the retrieved CO 2 abundance. The histograms presented in Figure 5 show that the retrieved abundances are consistent for each of the combined spectra, suggesting that the impact of cloud variability is not detectable with the resolution provided by JWST NIRSpec PRISM. This is further verified by the third panel, which shows consistent retrieved cloud top pressure for each spectra. While the cloud top pressure can be seen to vary in our models, this consistency in the retrieved cloud top pressures demonstrates that the precision of JWST NIRSpec PRISM will not be able to differentiate variable cloud spectra at any level of confidence. It can be seen from Figure 5 that for the CO 2 partial pressure greater than 10 −1 bars the posterior tends toward the upper prior, which is set by the physical limit of the volume mixing ratio, with the true value lying outside 1 σ . The lower partial pressures are not prior dominated and we are able to retrieve the correct volume mixing ratios within 1 σ . Further, the 10 cases for each partial pressure are consistent, suggesting that the variable clouds are not affecting the retrieved values. We are unable to constrain a water abundance due to its lack of strong spectral features in our models. Figure 5. Retrieved posterior distributions for four of the key parameters explored in this study. From top to bottom the four panels are: CO 2 abundance, H 2 O abundance, cloud top pressure, and temperature. Each colored histogram represents the retrieved parameter for one of the combined spectra (representing 10 different “observed” epochs), for a total 10 different combined spectra, each with different underlying cloud assumption. The thick solid vertical lines show the terminator-average abundance of CO 2 and H 2 O from the input models, while the dotted vertical lines represent