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<ri:Resource created="2024-04-05T07:34:04Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>New mean motion resonances with exoMMR package</title><shortName>J/AJ/166/94</shortName><identifier>ivo://CDS.VizieR/J/AJ/166/94</identifier><altIdentifier>doi:10.26093/cds/vizier.51660094</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>MacDonald M.G.</name></creator><creator><name>Polania Vivas M.S.</name></creator><creator><name>D'Angiolillo S.</name></creator><creator><name>Fernandez A.N.,Quinn T.</name></creator><date role="Updated">2025-04-11T20:10:22Z</date><date role="Created">2024-04-05T07:34:04Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>exoplanets</subject><subject>stellar-masses</subject><description>The study of orbital resonances allows for the constraint of planetary properties of compact systems. We can predict a system's resonances by observing the orbital periods of the planets, as planets in or near mean motion resonance (MMR) have period ratios that reduce to a ratio of small numbers. However, a period ratio near commensurability does not guarantee a resonance; we must study the system's dynamics and resonant angles to confirm resonance. Because resonances require in-depth study to confirm, and because two-body resonances require a measurement of the eccentricity vector which is quite challenging, very few resonant pairs or chains have been confirmed. We thus remain in the era of small-number statistics, not yet able to perform large population synthesis or informatics studies. To address this problem, we build a python package to find, confirm, and analyze MMRs, primarily through N-body simulations. We then analyze all near-resonant planets in the Kepler/K2 and TESS catalogs, confirming over 60 new resonant pairs and various new resonant chains. We additionally demonstrate the package's functionality and potential by characterizing the mass-eccentricity degeneracy of Kepler-80g, exploring the likelihood of an exterior giant planet in Kepler-80, and constraining the masses of planets in Kepler-305. We find that our methods overestimate the libration amplitudes of the resonant angles and struggle to confirm resonances in systems with more than three planets. We identify various systems that are likely resonant chains but that we are unable to confirm, and highlight next steps for exoplanetary resonances.</description><source format="bibcode">2023AJ....166...94M</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/166/94</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>IsServedBy</relationshipType><relatedResource>Conesearch service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/IV/38">IV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/750/114">J/ApJ/750/114 : Kepler TTVs. 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Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Np</name><description>[0/6] Number of confirmed planets modeled in the system</description><ucd>meta.number</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Npc</name><description>[2/6]? Number of planets modeled in the system if there are planet candidates</description><ucd>meta.number</ucd><dataType xsi:type="vs:VOTableType">int</dataType><flag>nullable</flag></column><column><name>Mass</name><description>[0.23/1.49] Stellar mass</description><unit>solMass</unit><ucd>phys.mass</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>E_Mass</name><description>[0.01/0.4]? 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Lower (or symmetric) uncertainty on Per</description><unit>d</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>t0</name><description>? mid-transit time, Barycentric Julian Date at TDB</description><unit>d</unit><ucd>time.epoch</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>E_t0</name><description>[0.0001/0.3]? Upper uncertainty on t0</description><unit>d</unit><ucd>stat.error;stat.max</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>e_t0</name><description>[0.0002/0.3]? Lower (or symmetric) uncertainty on t0</description><unit>d</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>Massp</name><description>[0.07/2161]? 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