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<ri:Resource created="2010-10-29T15:21:30Z" 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>T Tauri in and around bright-rimmed clouds</title><shortName>J/MNRAS/396/964</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/396/964</identifier><altIdentifier>doi:10.26093/cds/vizier.73960964</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Chauhan N.</name></creator><creator><name>Pandey A.K.</name></creator><creator><name>Ogura K.</name></creator><creator><name>Ojha D.K.</name></creator><creator><name>Bhatt B.C.</name></creator><creator><name>Ghosh S.K.,Rawat P.S.</name></creator><date role="Updated">2024-07-09T20:15:22Z</date><date role="Created">2010-10-29T15:21:30Z</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>molecular-clouds</subject><subject>pre-main-sequence-stars</subject><subject>infrared-photometry</subject><subject>millimeter-astronomy</subject><subject>photometry</subject><subject>submillimeter-astronomy</subject><description>The aim of this paper is to quantitatively testify the 'small-scale sequential star formation' hypothesis in and around bright-rimmed clouds (BRCs). As a continuation of the recent attempt by Ogura et al. (2007PASJ...59..199O), we have carried out BVIc photometry of four more BRC aggregates along with deeper re-observations of two previously observed BRCs. Again, quantitative age gradients are found in almost all the BRCs studied in the present work. 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