UVC surface fluxes for planets around all hosts from Kozakis et al. (2022) with modern N₂O (top) and with high and low N₂O abundances from this study with O₂ levels of 100% (second row), 10%, (third row), and 0.1% (bottom) PAL. The first panel in the top row indicates the top-of-the-atmosphere (TOA) flux for planets around all host stars, with the rest of the top row using the same y-axis limits for the corresponding O₂ values used in the bottom three rows to facilitate comparisons. Results for 1% PAL O₂ are extremely similar to those for 10% PAL O₂ and are therefore not included. The most significant changes in UVC surface flux occur in models with higher O₂ because the conversion from N₂O to NO_x is more efficient in higher O₂ environments. Larger amounts of NO_x have a greater impact on O₃ either by depleting it with NO_x catalytic cycles or producing it with the smog mechanism. While the results at 10% and 100% PAL O₂ tend to show increased O₃ shielding for low N₂O models, this trend reverses at 0.1% PAL O₂, where the low N₂O models consistently receive more surface UVC. This is because at low O₂ levels the effects of the smog mechanism become clearer as the Chapman mechanism is limited by the lack of O₂.