Fig. 3 demonstrates that the fluxes themselves are not small. The problem is seeing the planet from under the glare of the star (§\[telescopes\]). At 10 parsecs and an orbital separation of 0.05 AU, the maximum angular separation is a challenging $\sim$5 milliarcsecs.

Phase Functions for EGPs and Orbital Orientation {#phase}
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The planetary albedo and the phases executed as planets traverse their orbits are central quantities in the theory of EGP light curves. In addition, as we discuss in this section, the wavelength-dependent albedos are strong functions of orbital distance as well. Furthermore, the changing orientation of the illuminated face of a planet from the Earth’s perspective translates into a light curve that can show significant flux and color variations. In Fig. 2, these variations were averaged out over the orbit, assumed circular. The longitude independence of Jupiter’s $T/P$ profile results in little day/night variation in the mid-infrared and, hence, little phase variation, but such a planet is too cold to be self-luminous enough in the optical for its reflected component not to dominate at these shorter wavelengths. Hence, Jupiter’s optical fluxes can vary from superior conjunction (full face) to first quarter (90$^{\circ}$ from superior conjunction, not seen from 