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<ri:Resource created="2010-12-22T15:38:42Z" 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>Debris disks in NGC 2232</title><shortName>J/ApJ/688/597</shortName><identifier>ivo://CDS.VizieR/J/ApJ/688/597</identifier><altIdentifier>doi:10.26093/cds/vizier.16880597</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Currie T.</name></creator><creator><name>Plavchan P.</name></creator><creator><name>Kenyon S.J.</name></creator><date role="Updated">2017-09-29T09:03:54Z</date><date role="Created">2010-12-22T15:38:42Z</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>open-star-clusters</subject><subject>infrared-photometry</subject><subject>dwarf-stars</subject><subject>stellar-spectral-types</subject><subject>line-intensities</subject><subject>spectroscopy</subject><description>We describe Spitzer IRAC and MIPS observations of the nearby 25Myr old open cluster NGC 2232. Combining these data with ROSAT All-Sky Survey observations, proper motions, and optical photometry/spectroscopy, we construct a list of highly probable cluster members. We identify one A-type star, HD 45435, that has definite excess emission at 4.5-24um indicative of debris from terrestrial planet formation. We also identify 2-4 late-type stars with possible 8um excesses and 8 early-type stars with definite 24um excesses. Constraints on the dust luminosity and temperature suggest that the detected excesses are produced by debris disks. From our sample of B and A stars, stellar rotation appears to be correlated with 24um excess, a result that would be expected if massive primordial disks evolve into massive debris disks. To explore the evolution of the frequency and magnitude of debris around A-type stars, we combine our results with data for other young clusters.</description><source format="bibcode">2008ApJ...688..597C</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/688/597</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/IX/28">IX/28 : ROSAT HRI Pointed Observations (1RXH) (ROSAT Team, 2000)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/188/242">J/ApJS/188/242 : Variations on debris disks. II. 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