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<ri:Resource created="2026-08-07T10:16:02Z" status="active" updated="2026-09-14T14:05:09Z" 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>Warm Jupiter migration pathways. I. Radial veloc.</title><shortName>J/ApJS/280/76</shortName><identifier>ivo://CDS.VizieR/J/ApJS/280/76</identifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Morgan M.</name></creator><creator><name>Bowler B.P.</name></creator><creator><name>Tran Q.H.</name></creator><creator><name>Wittenmyer R.A.</name></creator><creator><name>Wright D.J.</name></creator><creator><name>Zhou G.,Fairnington T.R.</name></creator><date role="Updated">2026-09-14T14:05:09Z</date><date role="Created">2026-08-07T10:16:02Z</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-astronomy</subject><subject>spectroscopy</subject><subject>visible-astronomy</subject><subject>radial-velocity</subject><subject>astronomical-reference-materials</subject><subject>stellar-masses</subject><subject>metallicity</subject><subject>stellar-distance</subject><subject>stellar-spectral-types</subject><description>Giant planets are expected to predominantly form beyond the water-ice line and occasionally undergo inward migration. Unlike hot Jupiters, which can result from high-eccentricity tidal migration, warm Jupiters between 0.1 and 1au (~10-365days) are in many ways more challenging to explain because they reside outside the tidal influence of their host stars. Warm Jupiters should therefore preserve traces of their origins as their eccentricities are directly related to their past interactions. We analyze the eccentricities of 200 warm Jupiters orbiting 194 Sunlike host stars (with FGKM spectral types) using 18,587 radial velocity (RV) measurements across 40 high-resolution spectrographs. RVs are compiled from the literature and are supplemented with 540 new observations from MINERVA-Australis at Mount Kent Observatory and the Habitable-zone Planet Finder spectrograph at McDonald Observatory's Hobby-Eberly Telescope, which are timed to improve eccentricity constraints by sampling orbits near periastron passage. The overarching goal of this program is to establish the relative importance of giant planet migration channels through the largest homogeneous analysis of warm Jupiter orbital properties to date. In particular, we evaluate and compare the impact of different system architectures and host star characteristics on the population-level eccentricity distributions of warm Jupiters. Here, we present the target sample, observations, orbit-fitting procedure, and parameter summary statistics of our survey. All orbit fit solutions, parameter posterior chains, and merged RV tables for each system are made publicly available.</description><source format="bibcode">2025ApJS..280...76M</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/280/76</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/B/pastel">B/pastel : The PASTEL catalogue (Soubiran+, 2016-)</relatedResource><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/I/352">I/352 : Distances to 1.47 billion stars in Gaia EDR3 (Bailer-Jones+, 2021)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/V/137">V/137 : Extended Hipparcos Compilation (XHIP) (Anderson+, 2012)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/356/590">J/A+A/356/590 : The CORALIE survey for extrasolar planets II (Udry+, 2000)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/375/205">J/A+A/375/205 : The CORALIE survey for extrasolar planets V (Naef+ 2001)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/410/1039">J/A+A/410/1039 : Northern exoplanets ELODIE survey I (Perrier+, 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/398/363">J/A+A/398/363 : Statistical properties of exoplanets II (Santos+, 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/415/391">J/A+A/415/391 : CORALIE survey for extrasolar planets. 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