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<ri:Resource created="2016-01-05T10:17:13Z" 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>N131 bubble CO integrated intensity maps</title><shortName>J/A+A/585/A117</shortName><identifier>ivo://CDS.VizieR/J/A+A/585/A117</identifier><altIdentifier>doi:10.26093/cds/vizier.35850117</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Zhang C.-P.</name></creator><creator><name>Li G.-X.</name></creator><creator><name>Wyrowski F.</name></creator><creator><name>Wang J.-J.</name></creator><creator><name>Yuan J.-H.</name></creator><creator><name>Xu J.-L.,Gong Y.</name></creator><creator><name>Yeh C.C.</name></creator><creator><name>Menten K.M.</name></creator><date role="Updated">2016-01-05T09:18:01Z</date><date role="Created">2016-01-05T10:17:13Z</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>interstellar-medium</subject><subject>molecular-clouds</subject><subject>co-line-emission</subject><description>OB-type stars have strong ionizing radiation and drive energetic winds. The ultraviolet radiation from ionizing stars may heat dust and ionize gas to sweep up an expanding bubble shell. This shell may be the result of feedback leading to a new generation of stars. N131 is an infrared dust bubble residing in a molecular filament. We study the formation and fragmentation of this bubble with multiwavelength dust and gas observations. Towards the bubble N131, we analysed archival multiwavelength observations including 3.6, 4.5, 5.8, 8.0, 24, 70, 160, 250, 350, 500um, 1.1mm, and 21cm. 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