diameter\
$\lambda$ & $0.55$ $\mu$m & Central wavelength\
$\Delta \lambda$ & $0.11$ $\mu$m & Bandwidth\
IWA & $2\lambda/D$ (28.4 mas) & Inner working angle\
OWA & $15\lambda/D$ (213 mas) & Outer working angle\
$\zeta$ & $10^{-10}$ & Contrast level in detection region, relative to theoretical Airy peak\
$\Delta$mag$_{\rm floor}$ & $26$ & Systematic noise floor (i.e., dimmest point source detectable at S/N)\
$T$ & $0.2$ & End-to-end facility throughput\
S/N & $10$ & Signal to noise ratio required for broadband detection of a planet\
$F_0$ & $9500$ photons cm$^{-2}$ nm$^{-1}$ s$^{-1}$ & Flux zero-point at $V$ band\
$X$ & $0.7$ & Photometry aperture radius in $\lambda/D$\
$\Upsilon$ & $0.69$ & Fraction of Airy pattern contained within photometry aperture\
$\Omega$ & $\pi(X\lambda/D)^2$ radians & Solid angle subtended by photometry aperture\

Yield Maximization
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The estimated exoEarth candidate yield for a mission is equal to $\eta_{\earth}$ times the total completeness obtained for all observed stars within the assumed mission lifetime. Therefore, to calculate exoEarth candidate yield, one must decide which stars to observe, how long to observe them, and in what order, necessitating a target prioritization metric. Completeness $C$, the chance of observing an exoEarth candidate around a given star, can be 