$p$, but mostly in the blue and UV, where, however, chromophores can decrease it. The presence of clouds increases $p$ significantly. For instance, at 0.48 , Jupiter’s geometric albedo is $\sim$0.46 and Saturn’s is 0.39[@kark99]. Note that for orbital distances less than 1.5 AU, we expect the atmospheres of most EGPs to be clear. The albedo would be correspondingly low. As a consequence, the theoretical albedo is very non-monotonic with distance, ranging in the visible from perhaps $\sim$0.3 at 0.05 AU, to $\sim$0.05 at 0.2 AU, to $\sim$0.4 at 4 AU, to $\sim$0.7 at 15 AU [@bur.hub; @Sudarsky00; @Sudarsky03]. In the visible ($\sim$0.55 ), the geometric albedo for a roaster is severely suppressed by Na-D at 0.589 . Due to a methane feature, the geometric albedo can vary from 0.05 at $\sim$0.6 to $\sim$0.4 at 0.625 . Hence, variations with wavelength and with orbital distance by factors of 2 to 10 are not unexpected. Those planning programs of direct detection should be aware of such possibilities.

$\Phi(\alpha)$ and $p$ must be calculated or measured, but the sole dependence of $\Phi(\alpha)$ on $\alpha$ belies the complications introduced by an orbit’s inclination angle ($i$), eccentricity ($e$), argument of periastron ($\omega$), and longitude 