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<ri:Resource created="2026-09-02T15:31:03Z" status="active" updated="2026-09-02T14:32:46Z" version="1.2" 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/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>Kepler-1624b transit times from Kepler, LCOGT, &amp; WIRC</title><shortName>J/AJ/170/336</shortName><identifier>ivo://CDS.VizieR/J/AJ/170/336</identifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Im H.</name></creator><creator><name>Saidel M.</name></creator><creator><name>Knutson H.A.</name></creator><creator><name>Greklek-McKeon M.</name></creator><creator><name>Vissapragada S.,Collins K.A.</name></creator><creator><name>Fukui A.</name></creator><creator><name>Narita N.</name></creator><creator><name>Paragas K.</name></creator><creator><name>Schwarz R.P.</name></creator><creator><name>Shporer A.,Srdoc G.</name></creator><date role="Updated">2026-09-02T14:32:46Z</date><date role="Created">2026-09-02T15:31:03Z</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>infrared-photometry</subject><subject>visible-astronomy</subject><description>It is relatively rare for gas giant planets to have resonant or near-resonant companions, but these systems are particularly useful for constraining planet formation and migration models. In this study, we examine Kepler-1624b, a sub-Saturn orbiting an M dwarf that was previously found to exhibit transit timing variations (TTVs) with an amplitude of approximately 2 minutes, suggesting the presence of a nearby nontransiting companion. We reanalyze the transits from archival Kepler data and extend the TTV baseline by 11yr by combining TESS data with three new ground-based transit observations from Palomar and Las Cumbres Observatories. We jointly fit these datasets and find that the TTV amplitude is significantly weaker in our updated analysis. We calculate the Bayes factor for a one-planet versus two-planet model and find that the one-planet model is preferred. Our results highlight the need for careful analysis of systems with relatively low amplitude TTV signals that are identified in large automated catalogs.</description><source format="bibcode">2025AJ....170..336I</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/170/336</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>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/IV/39">IV/39 : TESS Input Catalog version 8.2 (TIC v8.2) (Paegert+, 2021)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/V/133">V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/771/129">J/ApJ/771/129 : Submillimetric Class II sources of Taurus (Andrews+, 2013)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/549/A109">J/A+A/549/A109 : HARPS XXXI. 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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>Inst</name><description>Instrument/source (Source) (1)</description><ucd>meta.id;instr</ucd><dataType xsi:type="vs:VOTableType" arraysize="14*">char</dataType></column><column><name>Epoch</name><description>[0/1367] Epoch number</description><ucd>time.epoch</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Tmid</name><description>[6109/10608] Observed midtime for epoch; BJD-2450000 (midtime)</description><unit>d</unit><ucd>time.epoch</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>e_Tmid</name><description>[3.9e-4/1.5e-3] Uncertainty in Tmid (e_midtime)</description><unit>d</unit><ucd>stat.error;time.epoch</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column></table></schema></tableset></ri:Resource>