The size of a planet is an observable property directly connected to the physics of its formation and evolution. We previously used precise radius measurements from the California-Kepler Survey (CKS) to detect a deficit in the distribution of planet radii between 1.5-2.0 R⊕. This gap splits the population of close-in (P < 100 d) small planets into two size regimes: Rp < 1.5 R⊕ and Rp = 2.0-3.0 R⊕, with few planets in between. The feature is predicted by several planet formation theories which can be tested by measuring the detailed characteristics of the radius gap. Here we rederive the stellar radii incorporating distance constraints available in the second data release from GAIA. With the higher precision stellar and planetary radii we measure the detailed shape and location of the gap and look for changes with respect to stellar type and incident flux.