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The chemical abundances of planet-hosting stars offer a glimpse into thecomposition of planet-forming environments. To further understand thisconnection, we make the first ever measurement of the correlation betweenplanet occurrence and chemical abundances for ten different elements (C, Mg,Al, Si, S, K, Ca, Mn, Fe, and Ni). Leveraging data from the Apache PointObservatory Galactic Evolution Experiment (APOGEE) and Gaia to derive precisestellar parameters ($\sigma_{R_\star}\approx2.3\%$,$\sigma_{M_\star}\approx4.5\%$) for a sample of 1,018 Kepler Objects ofInterest, we construct a sample of well-vetted Kepler planets with preciselymeasured radii ($\sigma_{R_p}\approx3.4\%$). After controlling for biases inthe Kepler detection pipeline and the selection function of the APOGEE survey,we characterize the relationship between planet occurrence and chemicalabundance as the number density of nuclei of each element in a star'sphotosphere raised to a power, $\beta$. $\beta$ varies by planet type, but isconsistent within our uncertainties across all ten elements. For hot planets($P$ = 1-10 days), an enhancement in any element of 0.1 dex corresponds to anincreased occurrence of $\approx$20% for Super-Earths ($R_p=1-1.9R_\oplus$) and$\approx$60% for Sub-Neptunes ($R_p=1.9-4R_\oplus$). Trends are weaker for warm($P$ = 10-100 days) planets of all sizes and for all elements, with thepotential exception of Sub-Saturns ($R_p=4-8R_\oplus$). Finally, we concludethis work with a caution to interpreting trends between planet occurrence andstellar age due to degeneracies caused by Galactic chemical evolution and makepredictions for planet occurrence rates in nearby open clusters to facilitatedemographics studies of young planetary systems.

The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets