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<ri:Resource created="2026-01-23T14:30:55Z" status="active" updated="2026-07-02T11:51:57Z" 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>TESS-Keck Survey. XXIV. 47 distant giants RVs</title><shortName>J/AJ/169/235</shortName><identifier>ivo://CDS.VizieR/J/AJ/169/235</identifier><altIdentifier>doi:10.26093/cds/vizier/be-59-7b</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Van Zandt J.</name></creator><creator><name>Petigura E.A.</name></creator><creator><name>Lubin J.</name></creator><creator><name>Weiss L.M.</name></creator><creator><name>Turtelboom E.V.,Fetherolf T.</name></creator><creator><name>Murphy J.M.A.</name></creator><creator><name>Crossfield I.J.M.</name></creator><creator><name>Gilbert G.J.</name></creator><creator><name>Mocnik T.,Batalha N.M.</name></creator><creator><name>Dressing C.</name></creator><creator><name>Fulton B.</name></creator><creator><name>Howard A.W.</name></creator><creator><name>Huber D.</name></creator><creator><name>Isaacson H.,Kane S.R.</name></creator><creator><name>Robertson P.</name></creator><creator><name>Roy A.</name></creator><creator><name>Angelo I.</name></creator><creator><name>Behmard A.</name></creator><creator><name>Beard C.,Chontos A.</name></creator><creator><name>Dai F.</name></creator><creator><name>Giacalone S.</name></creator><creator><name>Hill M.L.</name></creator><creator><name>Holcomb R.</name></creator><creator><name>Howell S.B.,Mayo A.W.</name></creator><creator><name>Pidhorodetska D.</name></creator><creator><name>Polanski A.S.</name></creator><creator><name>Rogers J.</name></creator><creator><name>Rosenthal L.J.,Rubenzahl R.A.</name></creator><creator><name>Scarsdale N.</name></creator><creator><name>Tyler D.</name></creator><creator><name>Yee S.W.</name></creator><creator><name>Zink J.</name></creator><date role="Updated">2026-07-02T11:51:57Z</date><date role="Created">2026-01-23T14:30:55Z</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>radial-velocity</subject><subject>visible-astronomy</subject><subject>spectroscopy</subject><subject>surveys</subject><subject>infrared-sources</subject><description>We present the results of the Distant Giants Survey, a 3yr radial velocity (RV) campaign to search for wide-separation giant planets orbiting Sun-like stars known to host an inner transiting planet. We defined a distant giant (DG) to have a=1-10AU and M_p_sin(i)=70-4000M_{Earth}_=0.2-12.5M_J_, and required transiting planets to have a&lt;1AU and R_p_=1-4R_{Earth}_. We assembled our sample of 47 stars using a single selection function and observed each star at monthly intervals to obtain ~30RV observations per target. The final catalog includes a total of 12 distant companions: four giant planets detected during our survey, two previously known giant planets, and six objects of uncertain disposition identified through RV/astrometric accelerations. Statistically, half of the uncertain objects are planets and the remainder are stars/brown dwarfs. We calculated target-by-target completeness maps to account for missed planets. We found evidence for a moderate enhancement of DGs in the presence of close-in small planets (CSs), P(DG|CS)=31_-11_^+12^%, over the field rate of P(DG)=16_-2_^+2^%. No enhancement is disfavored (p~8%). In contrast to a previous study, we found no evidence that stellar metallicity raises the enhancement of P(DG|CS) over P(DG). We found evidence that DG companions preferentially accompany shorter-period CS planets and have lower eccentricities than randomly selected giant planets. This points toward a nuanced picture of dynamically cool formation in which giants interact with, but do not disrupt, their inner systems.</description><source format="bibcode">2025AJ....169..235V</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/169/235</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/34">IV/34 : K2 Ecliptic Plane Input Catalog (EPIC) (Huber+, 2017)</relatedResource><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/I/355">I/355 : Gaia DR3 Part 1. 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