(scaled with stellar luminosity to maintain constant HZ temperature) and in eccentricity from $0$–$0.35$. The assumptions of this orbital distribution and the impact on yield will be addressed in a future paper. We assume the fraction of stars with an Earth-sized planet in the habitable zone is $\eta_{\Earth}=0.1$. Estimates of $\eta_{\Earth}$ include all habitable zone planets that are roughly Earth-sized—there is no guarantee that these planets are Earth-like. Strictly speaking, we calculate a yield of *candidate* exoEarths, a subset of which may be truly Earth-like.

Table \[baseline\_params\_table\] lists the baseline telescope and instrument parameters. We use optimistic parameters for a coronagraph under the assumption of a direct imaging mission several decades in the future. We ignore read noise and dark counts, implicitly requiring that future detector noise count rates be less than the astrophysical noise, and assume a diffraction-limited PSF.

We require a signal to noise ratio (S/N) of 10 for broadband detection. Given that the exposure time is proportional to S/N$^2$, this seemingly conservative assumption will negatively impact our yield estimates when compared to a S/N $\approx5$. However, @Kasdin:2006aa suggested that S/N $>7.1$ to ensure both a low false positive rate and low missed detection rate. Additionally, our exposure 