Dublin Core The Dublin Core metadata element set is common to all Omeka records, including items, files, and collections. For more information see, http://dublincore.org/documents/dces/. Title A name given to the resource Articles Article Faculty Publications -Articles Dublin Core The Dublin Core metadata element set is common to all Omeka records, including items, files, and collections. For more information see, http://dublincore.org/documents/dces/. Title A name given to the resource Properties and Occurrence Rates for Kepler Exoplanet Candidates as a Function of Host Star Metallicity from the DR25 Catalog Subject The topic of the resource methods: statistical; planets and satellites: formation; planets and satellites: general; stars: Abundances; stars: fundamental parameters Description An account of the resource Correlations between the occurrence rate of exoplanets and their host star properties provide important clues about the planet formation process. We studied the dependence of the observed properties of exoplanets (radius, mass, and orbital period) as a function of their host star metallicity. We analyzed the planetary radii and orbital periods of over 2800 Kepler candidates from the latest Kepler data release, DR25 (Q1-Q17), with revised planetary radii based on Gaia DR2 as a function of host star metallicity (from the Q1-Q17 (DR25) stellar and planet catalog). With a much larger sample and improved radius measurements, we are able to reconfirm previous results in the literature. We show that the average metallicity of the host star increases as the radius of the planet increases. We demonstrate this by first calculating the average host star metallicity for different radius bins and then supplementing these results by calculating the occurrence rate as a function of planetary radius and host star metallicity. We find a similar trend between host star metallicity and planet mass: the average host star metallicity increases with increasing planet mass. This trend, however, reverses for masses &gt;4.0 M J: host star metallicity drops with increasing planetary mass. We further examined the correlation between the host star metallicity and the orbital period of the planet. We find that for planets with orbital periods less than 10 days, the average metallicity of the host star is higher than that for planets with periods greater than 10 days. 2018. The American Astronomical Society. All rights reserved. Creator An entity primarily responsible for making the resource Narang M.; Manoj P.; Furlan E.; Mordasini C.; Henning T.; Mathew B.; Banyal R.K.; Sivarani T. Source A related resource from which the described resource is derived Astronomical Journal, Vol-156, No. 5 Publisher An entity responsible for making the resource available Institute of Physics Publishing Date A point or period of time associated with an event in the lifecycle of the resource 2018-01-01 Identifier An unambiguous reference to the resource within a given context <a href="https://doi.org/10.3847/1538-3881/aae391" target="_blank" rel="noreferrer noopener">https://doi.org/10.3847/1538-3881/aae391</a> <br /><br /><a href="https://www.scopus.com/inward/record.uri?eid=2-s2.0-85056722412&amp;doi=10.3847%2F1538-3881%2Faae391&amp;partnerID=40&amp;md5=b01679579f26285c2b5a9e292c931bdb" target="_blank" rel="noreferrer noopener">https://www.scopus.com/inward/record.uri?eid=2-s2.0-85056722412&amp;doi=10.3847%2f1538-3881%2faae391&amp;partnerID=40&amp;md5=b01679579f26285c2b5a9e292c931bdb</a> Rights Information about rights held in and over the resource All Open Access; Bronze Open Access; Green Open Access Relation A related resource ISSN: 46256 Format The file format, physical medium, or dimensions of the resource Online Language A language of the resource English Type The nature or genre of the resource Article Coverage The spatial or temporal topic of the resource, the spatial applicability of the resource, or the jurisdiction under which the resource is relevant Narang M., Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road, Colaba, Mumbai, 400005, India; Manoj P., Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road, Colaba, Mumbai, 400005, India; Furlan E., IPAC, Caltech, Mail Code 314-6, 1200 E. California Blvd., Pasadena, 91125, CA, United States; Mordasini C., Physikalisches Institut, Universitat Bern, Gesellschaftstrasse 6, Bern, 3012, Switzerland; Henning T., Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road, Colaba, Mumbai, 400005, India, Max-Planck-Institut f Astronomie, Kigstuhl 17, Heidelberg, D-69117, Germany; Mathew B., Department of Physics, Christ University, Hosur Road, Bangalore, 560029, India; Banyal R.K., Indian Institute of Astrophysics, Bangalore, 560034, India; Sivarani T., Indian Institute of Astrophysics, Bangalore, 560034, India