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<ri:Resource created="2026-04-15T14:59:15Z" status="active" updated="2026-05-04T07:43:19Z" 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>TI-DYE. II. HIP 67522 light curves &amp; transit data</title><shortName>J/ApJ/973/L30</shortName><identifier>ivo://CDS.VizieR/J/ApJ/973/L30</identifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Barber M.G.</name></creator><creator><name>Thao Pa C.</name></creator><creator><name>Mann A.W.</name></creator><creator><name>Vanderburg A.</name></creator><creator><name>Mori M.,Livingston J.H.</name></creator><creator><name>Fukui A.</name></creator><creator><name>Narita N.</name></creator><creator><name>Kraus A.L.</name></creator><creator><name>Tofflemire B.M.,Newton E.R.</name></creator><creator><name>Winn J.N.</name></creator><creator><name>Jenkins J.M.</name></creator><creator><name>Seager S.</name></creator><creator><name>Collins K.A.,Twicken J.D.</name></creator><date role="Updated">2026-05-04T07:43:19Z</date><date role="Created">2026-04-15T14:59:15Z</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><subject>young-stellar-objects</subject><description>The youngest (&lt;50Myr) planets are vital to understand planet formation and early evolution. The 17 Myr system HIP 67522 is already known to host a giant (~10R_{Earth}_) planet on a tight orbit. In their discovery paper, Rizzuto et al. reported a tentative single-transit detection of an additional planet in the system using TESS. Here, we report the discovery of HIP 67522c, a 7.9R_{Earth}_ planet that matches with that single-transit event. We confirm the signal with ground-based multiwavelength photometry from Sinistro and MuSCAT4. At a period of 14.33days, planet c is close to a 2:1 mean-motion resonance with b (6.96days or 2.06:1). The light curve shows distortions during many of the transits, which are consistent with spot-crossing events and/or flares. Fewer stellar activity events are seen in the transits of planet b, suggesting that planet c is crossing a more active latitude. Such distortions, combined with systematics in the TESS light-curve extraction, likely explain why planet c was previously missed.</description><source format="bibcode">2024ApJ...973L..30B</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/973/L30</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/34">IV/34 : K2 Ecliptic Plane Input Catalog (EPIC) (Huber+, 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/357">I/357 : Gaia DR3 Part 3. 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