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What determines the density structure of molecular clouds ? A case study of Orion B with Herschel

hal.structure.identifierFORMATION STELLAIRE 2013
dc.contributor.authorSCHNEIDER, N.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorANDRE, Ph.
dc.contributor.authorKONYVES, V.
hal.structure.identifierFORMATION STELLAIRE 2013
dc.contributor.authorBONTEMPS, Sylvain
hal.structure.identifierInstitut de Recherches sur les lois Fondamentales de l'Univers [IRFU]
dc.contributor.authorMOTTE, F.
dc.contributor.authorFEDERRATH, C.
hal.structure.identifierSchool of Physics and Astronomy [Cardiff]
dc.contributor.authorWARD-THOMPSON, D.
dc.contributor.authorARZOUMANIAN, D.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG ]
dc.contributor.authorBENEDETTINI, M.
dc.contributor.authorBRESSERT, E.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorDIDELON, P.
hal.structure.identifierHerzberg Institute of Astrophysics
dc.contributor.authorDI FRANCESCO, J.
hal.structure.identifierSchool of Physics and Astronomy [Cardiff]
dc.contributor.authorGRIFFIN, M.
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)]
dc.contributor.authorHILL, T.
dc.contributor.authorPALMEIRIM, P.
hal.structure.identifierIstituto di Fisica dello Spazio Interplanetario [IFSI]
dc.contributor.authorPEZZUTO, S.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorPERETTO, N.
hal.structure.identifierMilieux aquatiques, écologie et pollutions [UR MALY]
dc.contributor.authorROY, A.
dc.contributor.authorRYGL, K. L. J.
hal.structure.identifierAntarctic Research a European Network for Astrophysics [ARENA]
dc.contributor.authorSPINOGLIO, L.
hal.structure.identifierSTFC Rutherford Appleton Laboratory [RAL]
dc.contributor.authorWHITE, G.
dc.date.created2013-04-01
dc.date.issued2013
dc.identifier.issn2041-8205
dc.description.abstractEnA key parameter to the description of all star formation processes is the density structure of the gas. In this letter, we make use of probability distribution functions (PDFs) of Herschel column density maps of Orion B, Aquila, and Polaris, obtained with the Herschel Gould Belt survey (HGBS). We aim to understand which physical processes influence the PDF shape, and with which signatures. The PDFs of Orion B (Aquila) show a lognormal distribution for low column densities until Av 3 (6), and a power-law tail for high column densities, consistent with a rho r^-2 profile for the equivalent spherical density distribution. The PDF of Orion B is broadened by external compression due to the nearby OB stellar aggregates. The PDF of a quiescent subregion of the non-star-forming Polaris cloud is nearly lognormal, indicating that supersonic turbulence governs the density distribution. But we also observe a deviation from the lognormal shape at Av>1 for a subregion in Polaris that includes a prominent filament. We conclude that (i) the point where the PDF deviates from the lognormal form does not trace a universal Av-threshold for star formation, (ii) statistical density fluctuations, intermittency and magnetic fields can cause excess from the lognormal PDF at an early cloud formation stage, (iii) core formation and/or global collapse of filaments and a non-isothermal gas distribution lead to a power-law tail, and (iv) external compression broadens the column density PDF, consistent with numerical simulations.
dc.language.isoen
dc.publisherBristol : IOP Publishing
dc.title.enWhat determines the density structure of molecular clouds ? A case study of Orion B with Herschel
dc.typeArticle de revue
dc.identifier.doi10.1088/2041-8205/766/2/L17
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.arxiv1304.0327
bordeaux.journalThe Astrophysical journal letters
bordeaux.pageid. L17
bordeaux.volume766
bordeaux.issue2
bordeaux.peerReviewedoui
hal.identifierhal-00838712
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00838712v1
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