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Cluster-formation in the Rosette molecular cloud at the junctions of filaments

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.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.authorDIDELON, P.
dc.contributor.authorFEDERRATH, C.
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorBONTEMPS, Sylvain
hal.structure.identifierHerzberg Institute of Astrophysics
dc.contributor.authorDI FRANCESCO, J.
dc.contributor.authorARZOUMANIAN, D.
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.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.authorHILL, T.
dc.contributor.authorZAVAGNO, Annie
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorNGUYEN-LUONG, Q.
dc.contributor.authorATTARD, M.
hal.structure.identifierCentre d'étude spatiale des rayonnements [CESR]
dc.contributor.authorBERNARD, J. -Ph.
dc.contributor.authorELIA, D.
dc.contributor.authorFALLSCHEER, C.
hal.structure.identifierSchool of Physics and Astronomy [Cardiff]
dc.contributor.authorGRIFFIN, M.
dc.contributor.authorKIRK, J.
dc.contributor.authorKLESSEN, R.
dc.contributor.authorKÖNYVES, V.
dc.contributor.authorMARTIN, P.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorMEN'SHCHIKOV, A.
dc.contributor.authorPALMEIRIM, P.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorPERETTO, N.
dc.contributor.authorPESTALOZZI, M.
dc.contributor.authorRUSSEIL, D.
hal.structure.identifierHerzberg Institute of Astrophysics
dc.contributor.authorSADAVOY, S.
hal.structure.identifierCentre de Recherche Astrophysique de Lyon [CRAL]
dc.contributor.authorSOUSBIE, T.
hal.structure.identifierEuropean Southern Observatory [ESO]
dc.contributor.authorTESTI, L.
dc.contributor.authorTREMBLIN, Pascal
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.date.created2012-03-29
dc.date.issued2012
dc.identifier.issn0004-6361
dc.description.abstractEnFor many years feedback processes generated by OB-stars in molecular clouds, including expanding ionization fronts, stellar winds, or UV-radiation, have been proposed to trigger subsequent star formation. However, hydrodynamic models including radiation and gravity show that UV-illumination has little or no impact on the global dynamical evolution of the cloud. The Rosette molecular cloud, irradiated by the NGC2244 cluster, is a template region for triggered star-formation, and we investigated its spatial and density structure by applying a curvelet analysis, a filament-tracing algorithm (DisPerSE), and probability density functions (PDFs) on Herschel column density maps, obtained within the HOBYS key program. The analysis reveals not only the filamentary structure of the cloud but also that all known infrared clusters except one lie at junctions of filaments, as predicted by turbulence simulations. The PDFs of sub-regions in the cloud show systematic differences. The two UV-exposed regions have a double-peaked PDF we interprete as caused by shock compression. The deviations of the PDF from the log-normal shape typically associated with low- and high-mass star-forming regions at Av~3-4m and 8-10m, respectively, are found here within the very same cloud. This shows that there is no fundamental difference in the density structure of low- and high-mass star-forming regions. We conclude that star-formation in Rosette - and probably in high-mass star-forming clouds in general - is not globally triggered by the impact of UV-radiation. Moreover, star formation takes place in filaments that arose from the primordial turbulent structure built up during the formation of the cloud. Clusters form at filament mergers, but star formation can be locally induced in the direct interaction zone between an expanding HII--region and the molecular cloud.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enAstrophysics
dc.subject.enGalaxy Astrophysics
dc.title.enCluster-formation in the Rosette molecular cloud at the junctions of filaments
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201118566
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.arxiv1203.6472
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageL11
bordeaux.volume540
bordeaux.peerReviewedoui
hal.identifierhal-00685399
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00685399v1
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