Comparisons of 9.6 μm O₃ emission spectra features from Kozakis et al. (2022) with modern levels of CH₄ and N₂O (left) and O₃ features from varying CH₄ and N₂O models normalized to modern amounts of CH₄ and N₂O (right). Y-axis limits for all normalized features are the same to allow for comparison between different O₂ levels and host stars. For both variations in CH₄ and N₂O changes in the O₃ feature were primarily due to differences in O₃ abundance rather than changes in the atmospheric temperature profiles. The exception being for the CH₄ models for the hotter stars at 100% PAL O₂, which experienced stratospheric temperature changes depending on the amount of H₂O produced from CH₄.