9.6 µm O₃ feature for models from Kozakis et al. (2022) (left) and normalized models from varying N₂O (right) from simulated planetary emission spectra. Changes in the O₃ feature for this study depended primarily on changes in O₃ abundance – rather than on changes in the atmospheric temperature profile, as in Kozakis et al. (2022) – since varying N₂O often did not significantly impact the temperature profiles. As the K5V-hosted planet experienced the greatest change in O₃ abundance with the high N₂O models, it follows that its O₃ emission spectral features were the most impacted. The M5V-hosted planet experienced the smallest change in O₃ while varying N₂O, which is reflected by the small variations in its O₃ feature.