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The planet-metallicity correlation serves as a potential link betweenexoplanet systems as we observe them today and the effects of bulk compositionon the planet formation process. Many observers have noted a tendency forJovian planets to form around stars with higher metallicities; however, thereis no consensus on a trend for smaller planets. Here, we investigate theplanet-metallicity correlation for rocky planets in single and multi-planetsystems around Kepler M-dwarf and late K-dwarf stars. Due to molecularblanketing and the dim nature of these low mass stars, it is difficult to makedirect elemental abundance measurements via spectroscopy. We instead use acombination of accurate and uniformly measured parallaxes and photometry toobtain relative metallicities and validate this method with a subsample ofspectroscopically determined metallicities. We use the Kolmogorov-Smirnov (KS)test, Mann-Whitney U test, and Anderson-Darling test to compare the compactmultiple planetary systems with single transiting planet systems and systemswith no detected transiting planets. We find that the compact multipleplanetary systems are derived from a statistically more metal-poor population,with a p-value of 0.015 in the KS test, a p-value of 0.005 in the Mann-WhitneyU test, and a value of 2.574 in the Anderson-Darling test statistic, whichexceeds the derived threshold for significance by a factor of 25. We concludethat metallicity plays a significant role in determining the architecture ofrocky planet systems. Compact multiples either form more readily, or are morelikely to survive on Gyr timescales, around metal-poor stars.

Higher Compact Multiple Occurrence Around Metal-Poor M-Dwarfs and Late K-Dwarfs