various distances from a G2V star like the Sun. These models are the same as those depicted in Fig. 1. Similar plots for different assumed parameters can be generated. The water absorption troughs are manifest throughout. For the closer EGPs at higher atmospheric temperatures, carbon resides in CO and methane features are weak. For these close-in EGPs, the Na-D line at 0.589 and the corresponding resonance line of K I at 0.77 are important absorbers, suppressing flux in the visible bands. Otherwise, the optical flux is buoyed by Rayleigh scattering of stellar light. As $a$ increases, methane forms and the methane absorption features in the optical (most of the undulations seen in Fig. 2 for $a$  0.5 AU shortward of 1 ), at $\sim$3.3 , and at $\sim$7.8 appear. Concomitantly, Na and K disappear from the atmosphere and the fluxes from $\sim$1.5 to $\sim$4 drop. For all models, the mid-infrared fluxes longward of $\sim$4 are due to self-emission, not reflection. As Fig. 2 makes clear, for larger orbital distances a bifurcation between a reflection component in the optical and an emission component in the mid-infrared appears. This separation into components is not so straightforward for the closer, more massive, or 