do not significantly impact yield or target prioritization and require significant computational effort. On the other hand, the conventional treatment of exozodiacal dust as a uniform surface brightness independent of stellar type unfairly penalizes late type stars. We chose to define 1 “zodi" of dust as a constant habitable zone optical depth defined at the Earth-equivalent insolation distance, such that the exozodiacal surface brightness at wavelength $\lambda$, $I_{\rm EZ}(\lambda) \propto 10^{-0.4 M_{\lambda}^{\star}}/L_{\star}$, where $M_{\lambda}^{\star}$ is the absolute stellar magnitude at wavelength $\lambda$ and $L_{\star}$ is the bolometric stellar luminosity. Using this definition, yields are negligibly increased, but $\sim15\%$ more K and M dwarf type stars are observed.

Defining a Yield Goal {#yield_goals_section}
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Given the caveats detailed in Section \[caveats\], the absolute yield numbers presented in this work will undoubtedly change as our calculations advance and our understanding of the assumptions improve. We emphasize that the absolute yield numbers are sensitive to quantities that we do not vary in detail: poorly constrained astrophysical quantities, like $\eta_{\Earth}$ and the typical exoEarth candidate albedo, as well as assumed telescope and instrument parameters, like the required SNR for detection and the system throughput. *Rather than the absolute exoEarth candidate yield numbers, the primary 