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Recently, several groups have resolved a gap that bifurcates planets betweenthe size of Earth and Neptune into two populations. The location and depth ofthis feature is an important signature of the physical processes that form andsculpt planets. In particular, planets residing in the radius gap are valuableprobes of these processes as they may be undergoing the final stages ofenvelope loss. Here, we discuss two views of the radius gap by Fulton &Petigura (2018; F18) and Van Eylen et al. (2018; V18). In V18, the gap is widerand more devoid of planets. This is due, in part, to V18's more precisemeasurements of planet radius $R_p$. Thanks to Gaia, uncertainties in stellarradii Rstar are no longer the limiting uncertainties in determining $R_p$ forthe majority of Kepler planets; instead, errors in $R_p/R_\star$ dominate.V18's analysis incorporated short-cadence photometry along with constraints onmean stelar density that enabled more accurate determinations of $R_p/R_\star$.In the F18 analysis, less accurate $R_p/R_\star$ blurs the boundary the radiusgap. The differences in $R_p/R_\star$ are largest at high impact parameter ($b\gtrsim 0.8$) and often exceed 10%. This motivates excluding high-$b$ planetsfrom demographic studies, but identifying such planets from long-cadencephotometry alone is challenging. We show that transit duration can serve as aneffective proxy, and we leverage this information to enhance the contrastbetween the super-Earth and sub-Neptune populations.

Two Views of the Radius Gap and the Role of Light Curve Fitting