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We demonstrate that planet occurrence does not depend on stellargalactocentric velocity in the Solar neighborhood. Using Gaia DR2 astrometryand radial velocity data, we calculate 3D galactocentric velocities for 197,090Kepler field stars, 1647 of which are confirmed planet hosts. When we comparethe galactocentric velocities of planet hosts to those of the entire field starsample, we observe a statistically significant (KS p-value = $10^{-70}$)distinction, with planet hosts being apparently slower than field stars by$\sim$40 km/s. We explore some potential explanations for this difference andconclude that it is not a consequence of the planet-metallicity relation ordistinctions in the samples' thin/thick disk membership, but rather an artefactof Kepler's selection function. Non Kepler-host stars that have nearlyidentical distances, temperatures, surface gravities, and Kepler magnitudes tothe confirmed planet hosts also have nearly identical velocity distributions.Using one of these identical non-host samples, we consider that the probabilityof a star with velocity $v_{\mathrm{tot}}$ hosting a planet can be described byan exponential function proportional to $e^{(-v_{\mathrm{tot}}/v_0)}$. Using aMarkov Chain Monte Carlo sampler, we determine that $v_0 > $976 km/s to 99%confidence, which implies that planets in the Solar neighborhood are just aslikely to form around fast stars as they are around slow stars. Our workhighlights the subtle ways in which selection biases can create strongcorrelations without physical underpinnings.

Not Gone with the Wind: Planet Occurrence is Independent of Stellar Galactocentric Velocity