The host star fluxes at the location of a T_eq = 3000 K planet used to irradiate our planet atmosphere models (solid) compared to blackbodies of the same T_eff (dashed). While the total incoming stellar energy is equal, the A0 star (T_eff = 10,500 K) emits about half of its energy in the UV and has a prominent Balmer jump, while the G2 star (T_eff = 5700 K) generally emits the vast majority of its energy at visible and IR wavelengths and exhibits deeper absorption lines.