The radius distribution prior that was used in this work. The black histogram is the completeness-corrected single planet radius distribution from B. J. Fulton et al. (2017). The dashed blue is the model radius distribution that was used as our prior. The model fit did not include planets in the range of 1.5–2.0 R_⊕, making the prior agnostic to the presence of the radius gap. A prior that included the radius gap would differ by a factor of ∼2 within the radius gap range. The model used in this work imposes the constraint that small planets are more numerous than large planets and are therefore more probable to occur. Since a planet’s inferred radius is different depending on the host star, we used this to assign prior probabilities of a planet being circumprimary vs. circumsecondary.