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The Herschel view of star formation in the Rosette molecular cloud under the influence of NGC 2244

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)]
hal.structure.identifierInstitut de Recherches sur les lois Fondamentales de l'Univers [IRFU]
dc.contributor.authorMOTTE, F.
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
hal.structure.identifierUniversité Sciences et Technologies - Bordeaux 1 [UB]
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
dc.contributor.authorBONTEMPS, Sylvain
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorHENNEMANN, M.
dc.contributor.authorDIFRANCESCO, J.
dc.contributor.authorANDR, Ph.
hal.structure.identifierLaboratoire d'Astrophysique de Marseille [LAM]
hal.structure.identifierObservatoire Astronomique de Marseille Provence [OAMP]
dc.contributor.authorZAVAGNO, Annie
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.authorMEN'SHCHIKOV, A.
hal.structure.identifierInstitut d'astrophysique spatiale [IAS]
dc.contributor.authorABERGEL, A.
hal.structure.identifierLaboratoire d'Astrophysique de Marseille [LAM]
dc.contributor.authorBALUTEAU, J. -P.
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
dc.contributor.authorBERNARD, J. -Ph.
dc.contributor.authorCOX, P.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorDIDELON, P.
dc.contributor.authorDIGIORGIO, A. -M
hal.structure.identifierDépartement d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée [DAPNIA]
dc.contributor.authorGASTAUD, R.
hal.structure.identifierSchool of Physics and Astronomy [Cardiff]
dc.contributor.authorGRIFFIN, M.
dc.contributor.authorHARGRAVE, P.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorHILL, T.
hal.structure.identifierNational Astronomical Observatories [Beijing] [NAOC]
dc.contributor.authorHUANG, M.
hal.structure.identifierSchool of Physics and Astronomy [Cardiff]
dc.contributor.authorKIRK, J.
dc.contributor.authorKONYVES, V.
hal.structure.identifierSTFC Rutherford Appleton Laboratory [RAL]
dc.contributor.authorLEEKS, S.
hal.structure.identifierNational Astronomical Observatories [Beijing] [NAOC]
dc.contributor.authorLI, J. Z.
dc.contributor.authorMARSTON, A.
hal.structure.identifierCITA
dc.contributor.authorMARTIN, P.
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.
hal.structure.identifierIstituto di Fisica dello Spazio Interplanetario [IFSI]
dc.contributor.authorMOLINARI, S.
hal.structure.identifierStockholm University
dc.contributor.authorOLOFSSON, G.
dc.contributor.authorPANUZZO, P.
hal.structure.identifierIstituto di Fisica dello Spazio Interplanetario [IFSI]
dc.contributor.authorPERSI, P.
hal.structure.identifierIstituto di Fisica dello Spazio Interplanetario [IFSI]
dc.contributor.authorPEZZUTO, S.
hal.structure.identifierInstitut d'Astrophysique de Paris [IAP]
dc.contributor.authorROUSSEL, Hervé
hal.structure.identifierLaboratoire d'Astrophysique de Marseille [LAM]
dc.contributor.authorRUSSEIL, D.
hal.structure.identifierHerzberg Institute of Astrophysics
dc.contributor.authorSADAVOY, S.
hal.structure.identifierIstituto di Fisica dello Spazio Interplanetario [IFSI]
dc.contributor.authorSARACENO, P.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorSAUVAGE, M.
hal.structure.identifierRoyal Observatory Edinburgh [ROE]
dc.contributor.authorSIBTHORPE, B.
hal.structure.identifierAntarctic Research a European Network for Astrophysics [ARENA]
dc.contributor.authorSPINOGLIO, L.
dc.contributor.authorTESTI, L
hal.structure.identifierHerschel Science Center [Madrid]
dc.contributor.authorTEYSSIER, D.
dc.contributor.authorVAVREK, R.
hal.structure.identifierSchool of Physics and Astronomy [Cardiff]
dc.contributor.authorWARD-THOMPSON, D.
hal.structure.identifierSTFC Rutherford Appleton Laboratory [RAL]
dc.contributor.authorWHITE, G.
dc.contributor.authorWILSON, C. D.
dc.contributor.authorWOODCRAF, A.
dc.date.created2010-05-21
dc.date.issued2010
dc.identifier.issn0004-6361
dc.description.abstractEnThe Rosette molecular cloud is promoted as the archetype of a triggered star-formation site. This is mainly due to its morphology, because the central OB cluster NGC 2244 has blown a circular-shaped cavity into the cloud and the expanding HII-region now interacts with the cloud. Studying the spatial distribution of the different evolutionary states of all star-forming sites in Rosette and investigating possible gradients of the dust temperature will help to test the 'triggered star-formation' scenario in Rosette. We use continuum data obtained with the PACS (70 and 160 micron) and SPIRE instruments (250, 350, 500 micron) of the Herschel telescope during the Science Demonstration Phase of HOBYS. Three-color images of Rosette impressively show how the molecular gas is heated by the radiative impact of the NGC 2244 cluster. A clear negative temperature gradient and a positive density gradient (running from the HII-region/molecular cloud interface into the cloud) are detected. Studying the spatial distribution of the most massive dense cores (size scale 0.05 to 0.3 pc), we find an age-sequence (from more evolved to younger) with increasing distance to the cluster NGC 2244. No clear gradient is found for the clump (size-scale up to 1 pc) distribution. The existence of temperature and density gradients and the observed age-sequence imply that star formation in Rosette may indeed be influenced by the radiative impact of the central NGC 2244 cluster. A more complete overview of the prestellar and protostellar population in Rosette is required to obtain a firmer result.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enAstrophysics
dc.subject.enGalaxy Astrophysics
dc.title.enThe Herschel view of star formation in the Rosette molecular cloud under the influence of NGC 2244
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201014627
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.arxiv1005.3924
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageL83
bordeaux.volume518
bordeaux.peerReviewedoui
hal.identifierhal-00496008
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00496008v1
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