Earth’s reflectance by 50%. The Earth’s true phase function is non-Lambertian, with a number of processes increasing the reflectance in crescent phases [@2010ApJ...721L..67R]. Including these processes would lead to higher exoEarth candidate yield, but we avoided including these effects because there is no guarantee that exoEarth candidates would have atmospheres identical to Earth’s. The albedos and phase functions for exoEarth candidates may be the largest source of astrophysical uncertainty for exoEarth yield calculations. We found yield is roughly $\propto A_G^{0.8}$ for our baseline mission assuming Lambertian spheres.

We implemented a new treatment of the local zodiacal light. We calculated the zodiacal surface brightness for each target star as a function of ecliptic latitude. We found that as long as observations are made at solar longitudes $\gtrsim90^{\circ}$, the conventional treatment (a uniform zodiacal surface brightness of 23 mag arcsec$^{-2}$) is adequate. Our more realistic treatment did not significantly impact exoEarth candidate yield for the baseline mission, though it did slightly alter the prioritization of observed stars.

Finally, we investigated the assumptions that go into the calculation of exozodiacal light. We found that complex estimates of exozodiacal light that self-consistently calculate the exozodi surface brightness with the planet’s orbital orientation and phase 