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The planets are between the size of Uranus and Saturn at\u00a0 7.0\u00a0\u00b1\u00a00.2 \u00a0<jats:inline-formula>\n                     <jats:tex-math>\n\n<\/jats:tex-math>\n                     <jats:inline-graphic xmlns:xlink=\"http:\/\/www.w3.org\/1999\/xlink\" xlink:href=\"ajab5220ieqn1.gif\" xlink:type=\"simple\"\/>\n                  <\/jats:inline-formula> and\u00a0 4.1\u00a0\u00b1\u00a00.2  <jats:inline-formula>\n                     <jats:tex-math>\n\n<\/jats:tex-math>\n                     <jats:inline-graphic xmlns:xlink=\"http:\/\/www.w3.org\/1999\/xlink\" xlink:href=\"ajab5220ieqn2.gif\" xlink:type=\"simple\"\/>\n                  <\/jats:inline-formula>, respectively, and reside a mere 0.1% outside the nominal 3:2 mean-motion resonance. They represent a different outcome of the planet formation process than the solar system, as well as the vast majority of known exoplanets. We measured the physical and orbital properties of these planets using photometry from <jats:italic>K2<\/jats:italic>, <jats:italic>Spitzer<\/jats:italic>, and ground-based telescopes, along with radial velocities from Keck\/HIRES. Through a joint photodynamical model, we found that the planets have moderate eccentricities of <jats:italic>e<\/jats:italic>\u00a0\u2248\u00a00.20 and well-aligned apsides \u0394<jats:italic>\u03d6<\/jats:italic>\u00a0\u2248\u00a00\u00b0. The planets occupy a strictly nonresonant configuration: the resonant angles circulate rather than librate. This defies the predictions of standard formation pathways that invoke convergent or divergent migration, both of which predict \u0394<jats:italic>\u03d6<\/jats:italic>\u00a0\u2248\u00a0180\u00b0 and eccentricities of a few percent or less. We measured masses of <jats:italic>M<\/jats:italic>\n                  <jats:sub>\n                     <jats:italic>p<\/jats:italic>,<jats:italic>b<\/jats:italic>\n                  <\/jats:sub>\u00a0=  32.4\u00a0\u00b1\u00a01.7  <jats:inline-formula>\n                     <jats:tex-math>\n\n<\/jats:tex-math>\n                     <jats:inline-graphic xmlns:xlink=\"http:\/\/www.w3.org\/1999\/xlink\" xlink:href=\"ajab5220ieqn3.gif\" xlink:type=\"simple\"\/>\n                  <\/jats:inline-formula> and <jats:italic>M<\/jats:italic>\n                  <jats:sub>\n                     <jats:italic>p<\/jats:italic>,<jats:italic>c<\/jats:italic>\n                  <\/jats:sub>\u00a0=\u00a0 10.8\u00a0\u00b1\u00a00.6  <jats:inline-formula>\n                     <jats:tex-math>\n\n<\/jats:tex-math>\n                     <jats:inline-graphic xmlns:xlink=\"http:\/\/www.w3.org\/1999\/xlink\" xlink:href=\"ajab5220ieqn4.gif\" xlink:type=\"simple\"\/>\n                  <\/jats:inline-formula>. Our measurements, with 5% fractional uncertainties, are among the most precise of any sub-Jovian exoplanet. Mass and size reflect a planet\u2019s core\/envelope structure. Despite having a relatively massive core of <jats:inline-formula>\n                     <jats:tex-math>\n\n<\/jats:tex-math>\n                     <jats:inline-graphic xmlns:xlink=\"http:\/\/www.w3.org\/1999\/xlink\" xlink:href=\"ajab5220ieqn5.gif\" xlink:type=\"simple\"\/>\n                  <\/jats:inline-formula>\u00a0\u2248\u00a015 <jats:inline-formula>\n                     <jats:tex-math>\n\n<\/jats:tex-math>\n                     <jats:inline-graphic xmlns:xlink=\"http:\/\/www.w3.org\/1999\/xlink\" xlink:href=\"ajab5220ieqn6.gif\" xlink:type=\"simple\"\/>\n                  <\/jats:inline-formula>, K2-19b is envelope-rich, with an envelope mass fraction of roughly 50%. This planet poses a challenge to standard models of core-nucleated accretion, which predict that cores \u227310 <jats:inline-formula>\n                     <jats:tex-math>\n\n<\/jats:tex-math>\n                     <jats:inline-graphic xmlns:xlink=\"http:\/\/www.w3.org\/1999\/xlink\" xlink:href=\"ajab5220ieqn7.gif\" xlink:type=\"simple\"\/>\n                  <\/jats:inline-formula> will quickly accrete gas and trigger runaway accretion when the envelope mass exceeds that of the core.<\/jats:p>","DOI":"10.3847\/1538-3881\/ab5220","type":"journal-article","created":{"date-parts":[[2019,12,10]],"date-time":"2019-12-10T20:13:13Z","timestamp":1576008793000},"page":"2","update-policy":"https:\/\/doi.org\/10.1088\/crossmark-policy","source":"Crossref","is-referenced-by-count":23,"title":["K2-19b and c are in a 3:2 Commensurability but out of Resonance: A Challenge to Planet Assembly by Convergent Migration"],"prefix":"10.3847","volume":"159","author":[{"ORCID":"https:\/\/orcid.org\/0000-0003-0967-2893","authenticated-orcid":false,"given":"Erik A.","family":"Petigura","sequence":"first","affiliation":[]},{"ORCID":"https:\/\/orcid.org\/0000-0002-4881-3620","authenticated-orcid":false,"given":"John","family":"Livingston","sequence":"additional","affiliation":[]},{"given":"Konstantin","family":"Batygin","sequence":"additional","affiliation":[]},{"ORCID":"https:\/\/orcid.org\/0000-0002-4535-6241","authenticated-orcid":false,"given":"Sean M.","family":"Mills","sequence":"additional","affiliation":[]},{"given":"Michael","family":"Werner","sequence":"additional","affiliation":[]},{"ORCID":"https:\/\/orcid.org\/0000-0002-0531-1073","authenticated-orcid":false,"given":"Howard","family":"Isaacson","sequence":"additional","affiliation":[]},{"ORCID":"https:\/\/orcid.org\/0000-0003-3504-5316","authenticated-orcid":false,"given":"Benjamin J.","family":"Fulton","sequence":"additional","affiliation":[]},{"ORCID":"https:\/\/orcid.org\/0000-0001-8638-0320","authenticated-orcid":false,"given":"Andrew W.","family":"Howard","sequence":"additional","affiliation":[]},{"ORCID":"https:\/\/orcid.org\/0000-0002-3725-3058","authenticated-orcid":false,"given":"Lauren M.","family":"Weiss","sequence":"additional","affiliation":[]},{"ORCID":"https:\/\/orcid.org\/0000-0001-9513-1449","authenticated-orcid":false,"given":"N\u00e9stor","family":"Espinoza","sequence":"additional","affiliation":[]},{"ORCID":"https:\/\/orcid.org\/0000-0002-6227-7510","authenticated-orcid":false,"given":"Daniel","family":"Jontof-Hutter","sequence":"additional","affiliation":[]},{"ORCID":"https:\/\/orcid.org\/0000-0002-1836-3120","authenticated-orcid":false,"given":"Avi","family":"Shporer","sequence":"additional","affiliation":[]},{"ORCID":"https:\/\/orcid.org\/0000-0001-6023-1335","authenticated-orcid":false,"given":"Daniel","family":"Bayliss","sequence":"additional","affiliation":[]},{"given":"S. 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