times by increasing the background light. For each target star, we calculated stellar luminosity from the *Hipparcos* parallax data, *Hipparcos* Johnson $V$ and $B-V$ values, and bolometric corrections given by Equations 1 and 2 from @2012PASP..124..418T. As discussed in @2012PASP..124..418T, the *Hipparcos* catalog is incomplete for late type stars. Since late type stars have compact habitable zones, the *Hipparcos* incompleteness may lead to underestimation of exoEarth candidate yields for large apertures with small inner working angles.

Completeness calculator
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For exoEarth candidate yield, “completeness" is defined as the chance of observing an exoEarth candidate around a given star if that exoEarth candidate exists [@2004ApJ...607.1003B]. The chance of observing an exoEarth candidate is therefore the product of completeness and $\eta_{\earth}$. For an exoEarth candidate to be observable, it must appear exterior to the IWA of the instrument, interior to the outer working angle (OWA), and must be bright enough to observe at a given S/N within a given exposure time. Because we will know little about the majority of planetary systems prior to imaging them, completeness is calculated via a Monte Carlo simulation of all possible planets satisfying certain constraints.

We calculated single-visit obscurational and photometric completeness for each star in 