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<ri:Resource created="2009-07-03T08:34:16Z" 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>Stellar population in Chamaeleon I</title><shortName>J/ApJS/173/104</shortName><identifier>ivo://CDS.VizieR/J/ApJS/173/104</identifier><altIdentifier>doi:10.26093/cds/vizier.21730104</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Luhman K.L.</name></creator><date role="Updated">2017-07-11T13:09:29Z</date><date role="Created">2009-07-03T08:34:16Z</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>effective-temperature</subject><subject>infrared-photometry</subject><subject>visible-astronomy</subject><subject>photometry</subject><subject>extinction</subject><subject>pre-main-sequence-stars</subject><subject>young-stellar-objects</subject><description>I present a new census of the stellar population in the ChamaeleonI star-forming region. Using optical and near-IR photometry and follow-up spectroscopy, I have discovered 50 new members of ChamaeleonI, expanding the census of known members to 226 objects. Fourteen of these new members have spectral types later than M6, which doubles the number of known members that are likely to be substellar. I have estimated extinctions, luminosities, and effective temperatures for the known members, used these data to construct an H-R diagram for the cluster, and inferred individual masses and ages with the theoretical evolutionary models of Baraffe and Chabrier. The low-mass stars are more widely distributed than members at other masses in the northern subcluster, but this is not the case in the southern subcluster. Meanwhile, the brown dwarfs have the same spatial distribution as the stars out to a radius of 3{deg} (8.5pc) from the center of ChamaeleonI.</description><source format="bibcode">2007ApJS..173..104L</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/173/104</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/J/A+A/416/555">J/A+A/416/555 : Brown Dwarfs in ChaI Dark Cloud (Lopez-Marti+ 2004)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/124/1001">J/AJ/124/1001 : JHKs photometry of Cha I variables (Carpenter, 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