Comparisons of the 9.6 μm O₃ emission spectra feature for all hosts at different O₂ levels using modern levels of CH₄ (left) and O₃ features for different CH₄ abundances (right) normalized to features with modern levels of CH₄. Normalized O₃ features use the same y-axis limits for all host stars in order to compare the difference in impact of CH₄ on O₃ for different hosts. For the hottest hosts at 100% PAL O₂ changes in feature strength are due to changes in O₃ abundances as well as stratospheric temperatures differences from H₂O abundance, while the rest of the model spectra variations are due mainly to changes in O₃ due to variations in CH₄.