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The spine of the swan: A Herschel study of the DR21 ridge and filaments in Cygnus X

hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorHENNEMANN, M.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
hal.structure.identifierInstitut de Recherches sur les lois Fondamentales de l'Univers [IRFU]
dc.contributor.authorMOTTE, F.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorSCHNEIDER, N.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorDIDELON, P.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorHILL, T.
dc.contributor.authorARZOUMANIAN, D.
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorBONTEMPS, Sylvain
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorCSENGERI, T.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorANDRE, Ph.
dc.contributor.authorKONYVES, V.
hal.structure.identifierGroupe d'Etudes des Matériaux Hétérogènes [GEMH]
dc.contributor.authorLOUVET, François
dc.contributor.authorMARSTON, A.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorMEN'SHCHIKOV, A.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
hal.structure.identifierInstitut de Recherches sur les lois Fondamentales de l'Univers [IRFU]
dc.contributor.authorMINIER, V.
dc.contributor.authorLUONG, Q. Nguyen
dc.contributor.authorPALMEIRIM, P.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorPERETTO, N.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorSAUVAGE, M.
dc.contributor.authorZAVAGNO, Annie
dc.contributor.authorANDERSON, L. D.
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
dc.contributor.authorBERNARD, J. -Ph.
hal.structure.identifierHerzberg Institute of Astrophysics
dc.contributor.authorDI FRANCESCO, J.
dc.contributor.authorELIA, D.
hal.structure.identifierNational Astronomical Observatories [Beijing] [NAOC]
dc.contributor.authorLI, J. Z.
hal.structure.identifierLaboratoire de Modélisation Multi-échelles des Combustibles [LM2C]
dc.contributor.authorMARTIN, P. G.
hal.structure.identifierIstituto di Fisica dello Spazio Interplanetario [IFSI]
dc.contributor.authorMOLINARI, S.
hal.structure.identifierIstituto di Fisica dello Spazio Interplanetario [IFSI]
dc.contributor.authorPEZZUTO, S.
dc.contributor.authorRUSSEIL, D.
dc.contributor.authorRYGL, K. L. J.
dc.contributor.authorSCHISANO, E.
hal.structure.identifierAntarctic Research a European Network for Astrophysics [ARENA]
dc.contributor.authorSPINOGLIO, L.
hal.structure.identifierCentre de Recherche Astrophysique de Lyon [CRAL]
dc.contributor.authorSOUSBIE, T.
hal.structure.identifierSchool of Physics and Astronomy [Cardiff]
dc.contributor.authorWARD-THOMPSON, D.
hal.structure.identifierEngineering Department
dc.contributor.authorWHITE, G. J.
dc.date.created2012-06-06
dc.date.issued2012
dc.identifier.issn0004-6361
dc.description.abstractEnIn order to characterise the cloud structures responsible for the formation of high-mass stars, we present Herschel observations of the DR21 environment. Maps of the column density and dust temperature unveil the structure of the DR21 ridge and several connected filaments. The ridge has column densities larger than 1e23/cm^2 over a region of 2.3 pc^2. It shows substructured column density profiles and branching into two major filaments in the north. The masses in the studied filaments range between 130 and 1400 Msun whereas the mass in the ridge is 15000 Msun. The accretion of these filaments onto the DR21 ridge, suggested by a previous molecular line study, could provide a continuous mass inflow to the ridge. In contrast to the striations seen in e.g., the Taurus region, these filaments are gravitationally unstable and form cores and protostars. These cores formed in the filaments potentially fall into the ridge. Both inflow and collisions of cores could be important to drive the observed high-mass star formation. The evolutionary gradient of star formation running from DR21 in the south to the northern branching is traced by decreasing dust temperature. This evolution and the ridge structure can be explained by two main filamentary components of the ridge that merged first in the south.
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enThe spine of the swan: A Herschel study of the DR21 ridge and filaments in Cygnus X
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201219429
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.identifier.arxiv1206.1243
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageL3
bordeaux.volume543
bordeaux.peerReviewedoui
hal.identifierhal-00707804
hal.version1
hal.popularnon
hal.audienceNon spécifiée
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00707804v1
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