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We present independent and self-consistent metallicities for a sample of 807planet-hosting stars from the California-Kepler Survey from an LTEspectroscopic analysis using a selected sample of Fe I and Fe II lines.Correlations between host-star metallicities, planet radii, and planetaryarchitecture (orbital periods - warm or hot - and multiplicity - single ormultiple), were investigated using non-parametric statistical tests. Inaddition to confirming previous results from the literature, e.g., that overallhost star metallicity distributions differ between hot and warm planetarysystems of all types, we report on a new finding that when comparing the medianmetallicities of hot versus warm systems, the difference for multipleSuper-Earths is considerably larger when compared to that difference in singleSuper-Earths. The metallicity CDFs of hot single Super-Earths versus warmsingle Super-Earths indicate different parent stellar populations, while forSub-Neptunes this is not the case. The transition radius between Sub-Neptunesand Sub-Saturns was examined by comparing the APOGEE metallicity distributionfor the Milky Way thin disk in the solar neighborhood with metallicitydistributions of host stars segregated based upon the largest known planet intheir system. These comparisons reveal increasingly different metallicitydistributions as the radius of the largest planet in the systems increases,with the parent stellar metallicities becoming significantly different forR$_{p}>$ 2.7 R$_{\oplus}$. The behavior of the p-values as a function of planetradius undergoes a large slope change at R$_{p}$ = 4.4 $\pm$ 0.5 R$_{\oplus}$,indicating the radius boundary between small and large planets.

A Spectroscopic Analysis of the California-Kepler Survey Sample: II. Correlations of Stellar Metallicities with Planetary Architectures