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Herschel observations of embedded protostellar clusters in the Rosette Molecular Cloud

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.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
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.authorSCHNEIDER, N.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorCSENGERI, T.
hal.structure.identifierMax-Planck-Institut für Astronomie [MPIA]
dc.contributor.authorBALOG, Z.
hal.structure.identifierHerzberg Institute of Astrophysics
dc.contributor.authorDI FRANCESCO, J.
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.authorANDRÉ, Ph.
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.
dc.contributor.authorALI, B.
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.authorDI GIORGIO, A. -M.
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.identifierDépartement d'Astrophysique (ex SAP) [DAP]
dc.contributor.authorHOREAU, B.
hal.structure.identifierNational Astronomical Observatories [Beijing] [NAOC]
dc.contributor.authorHUANG, M.
hal.structure.identifierSchool of Physics and Astronomy [Cardiff]
dc.contributor.authorKIRK, J.
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.identifierIstituto di Fisica dello Spazio Interplanetario [IFSI]
dc.contributor.authorMOLINARI, S.
dc.contributor.authorLUONG, Q. Nguyen
hal.structure.identifierStockholm University
dc.contributor.authorOLOFSSON, G.
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.identifierLaboratoire d'Astrophysique de Marseille [LAM]
dc.contributor.authorRUSSEIL, D.
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.
hal.structure.identifierEuropean Southern Observatory [ESO]
dc.contributor.authorTESTI, L.
hal.structure.identifierSchool of Physics and Astronomy [Cardiff]
dc.contributor.authorWARD-THOMPSON, D.
hal.structure.identifierSTFC Rutherford Appleton Laboratory [RAL]
dc.contributor.authorWHITE, G.
hal.structure.identifierUniversity of Exeter
dc.contributor.authorWILSON, C.
hal.structure.identifierRoyal Observatory Edinburgh [ROE]
dc.contributor.authorWOODCRAFT, A.
dc.date.created2010-05-18
dc.date.issued2010
dc.identifier.issn0004-6361
dc.description.abstractEnThe Herschel OB young stellar objects survey (HOBYS) has observed the Rosette molecular cloud, providing an unprecedented view of its star formation activity. These new far-infrared data reveal a population of compact young stellar objects whose physical properties we aim to characterise. We compiled a sample of protostars and their spectral energy distributions that covers the near-infrared to submillimetre wavelength range. These were used to constrain key properties in the protostellar evolution, bolometric luminosity, and envelope mass and to build an evolutionary diagram. Several clusters are distinguished including the cloud centre, the embedded clusters in the vicinity of luminous infrared sources, and the interaction region. The analysed protostellar population in Rosette ranges from 0.1 to about 15 Msun with luminosities between 1 and 150 Lsun, which extends the evolutionary diagram from low-mass protostars into the high-mass regime. Some sources lack counterparts at near- to mid-infrared wavelengths, indicating extreme youth. The central cluster and the Phelps & Lada 7 cluster appear less evolved than the remainder of the analysed protostellar population. For the central cluster, we find indications that about 25% of the protostars classified as Class I from near- to mid-infrared data are actually candidate Class 0 objects. As a showcase for protostellar evolution, we analysed four protostars of low- to intermediate-mass in a single dense core, and they represent different evolutionary stages from Class 0 to Class I. Their mid- to far-infrared spectral slopes flatten towards the Class I stage, and the 160 to 70um flux ratio is greatest for the presumed Class 0 source. This shows that the Herschel observations characterise the earliest stages of protostellar evolution in detail.
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enHerschel observations of embedded protostellar clusters in the Rosette Molecular Cloud
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201014629
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.arxiv1005.3118
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageL84
bordeaux.volume518
bordeaux.peerReviewedoui
hal.identifierhal-00523477
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00523477v1
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