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<ri:Resource created="2025-02-25T14:22:35Z" status="active" updated="2025-05-21T20:14:25Z" 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>ALMA CO obs. of the 30 Dor molecular cloud complex</title><shortName>J/ApJ/932/47</shortName><identifier>ivo://CDS.VizieR/J/ApJ/932/47</identifier><altIdentifier>doi:10.26093/cds/vizier.19320047</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Wong T.</name></creator><creator><name>Oudshoorn L.</name></creator><creator><name>Sofovich E.</name></creator><creator><name>Green A.</name></creator><creator><name>Shah C.</name></creator><creator><name>Indebetouw R.,Meixner M.</name></creator><creator><name>Hacar A.</name></creator><creator><name>Nayak O.</name></creator><creator><name>Tokuda K.</name></creator><creator><name>Bolatto A.D.</name></creator><creator><name>Chevance M.,De Marchi G.</name></creator><creator><name>Fukui Y.</name></creator><creator><name>Hirschauer A.S.</name></creator><creator><name>Jameson K.E.</name></creator><creator><name>Kalari V.,Lebouteiller V.</name></creator><creator><name>Looney L.W.</name></creator><creator><name>Madden S.C.</name></creator><creator><name>Onishi T.</name></creator><creator><name>Roman-Duval J.,Rubio M.</name></creator><creator><name>Tielens A.G.G.M.</name></creator><date role="Updated">2025-05-21T20:14:25Z</date><date role="Created">2025-02-25T14:22:35Z</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>magellanic-clouds</subject><subject>star-forming-regions</subject><subject>molecular-clouds</subject><subject>co-line-emission</subject><subject>interstellar-medium</subject><description>We present results of a wide-field (approximately 60x90pc) Atacama Large Millimeter/submillimeter Array mosaic of CO(2-1) and ^13^CO(2-1) emission from the molecular cloud associated with the 30 Doradus star-forming region in the Large Magellanic Cloud (LMC). Three main emission complexes, including two forming a bow-tie-shaped structure extending northeast and southwest from the central R136 cluster, are resolved into complex filamentary networks. Consistent with previous studies, we find that the central region of the cloud has higher line widths at a fixed size relative to the rest of the molecular cloud and to other LMC clouds, indicating an enhanced level of turbulent motions. However, there is no clear trend in gravitational boundedness (as measured by the virial parameter) with distance from R136. Structures observed in 13CO are spatially coincident with filaments and are close to a state of virial equilibrium. In contrast, 12CO structures vary greatly in virialization, with low CO surface brightness structures outside of the main filamentary network being predominantly unbound. The low surface brightness structures constitute ~10% of the measured CO luminosity; they may be shredded remnants of previously star-forming gas clumps, or alternatively the CO-emitting parts of more massive, CO-dark structures.</description><source format="bibcode">2022ApJ...932...47W</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/932/47</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/II/305">II/305 : SAGE LMC and SMC IRAC Source Catalog (IPAC 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/136/18">J/AJ/136/18 : LMC SAGE. 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(Wong+, 2011)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/558/A134">J/A+A/558/A134 : VLT-FLAMES Tarantula Survey. 30Dor stars (Doran+, 2013)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/774/73">J/ApJ/774/73 : ALMA CO observations of 30 Dor (Indebetouw+, 2013)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/148/124">J/AJ/148/124 : Herschel key program Heritage (Seale+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/574/A13">J/A+A/574/A13 : VFTS. B-type stars classification and RV (Evans+, 2015)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/222/11">J/ApJS/222/11 : Hubble Tarantula Treasury Project (HTTP). III. (Sabbi+, 2016)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/156/98">J/AJ/156/98 : Runaway stars in the 30 Dor region of the LMC (Platais+, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/621/A62">J/A+A/621/A62 : 4 LMC SFRs velocity profile maps (Okada+, 2019)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/500/4257">J/MNRAS/500/4257 : Dense cores in Serpens region from HGBS (Fiorellino+, 2021)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/503/292">J/MNRAS/503/292 : NIR photometry of the core of R136 (Khorrami+, 2021)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/649/L8">J/A+A/649/L8 : Extreme adaptive optics astrometry of R136 (Khorrami+, 2021)</relatedResource></relationship></content><rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</rights><capability><interface xsi:type="vr:WebBrowser"><accessURL 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