revisits in this study. Revisits can both increase and decrease mission yield. In the event that an exoEarth is not detected around a given star, revisiting that star at a later time, after any potential exoEarths have had a chance to move along their orbits, could result in a new detection. On the other hand, revisits will also be required to establish common proper motion and constrain the orbit of any detected exoEarth candidates, reducing the amount of time available for new exoEarth candidate detections around other stars. A proper calculation of how revisits impact mission yield requires optimizing the time between visits, which is work that we leave for future development. Because we do not include revisits, we place no restriction on the maximum exposure time for single-visit detection.

The astrophysical parameters assumed for our baseline study are listed in Table \[exoearth\_params\_table\]. We choose $\eta_{\Earth} = 0.1$, consistent with recent estimates ranging from $\sim$ 0.05 – 0.2 for Sun-like stars [@2013PNAS..11019273P; @2014arXiv1404.2960M; @Silburt:2014aa]. We assume all exoEarth candidates are Earth twins, an assumption we address in Appendix \[earth\_albedo\_appendix\]. We use the same habitable zone conventions as @2005ApJ...624.1010B, distributing all planets uniformly and linearly in semi-major axis from $0.7$–$1.5$ AU 