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Detection of two power-law tails in the probability distribution functions of massive GMCs

hal.structure.identifierFORMATION STELLAIRE 2015
hal.structure.identifierUniversität zu Köln = University of Cologne
dc.contributor.authorSCHNEIDER, N.
hal.structure.identifierFORMATION STELLAIRE 2015
dc.contributor.authorBONTEMPS, Sylvain
hal.structure.identifierMax-Planck-Institut für Astrophysik [MPA]
dc.contributor.authorGIRICHIDIS, P.
hal.structure.identifierSchool of Physics and Astronomy [Cardiff]
dc.contributor.authorRAYNER, T.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorMOTTE, F.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorANDRÉ, P.
hal.structure.identifierLaboratoire d'Astrophysique de Marseille [LAM]
dc.contributor.authorRUSSEIL, D.
hal.structure.identifierInstitut d'astrophysique spatiale [IAS]
dc.contributor.authorABERGEL, A.
hal.structure.identifierNational Radio Astronomy Observatory [Green Bank] [NRAO]
hal.structure.identifierDepartment of Physics and Astronomy [Morgantown]
dc.contributor.authorANDERSON, L.
hal.structure.identifierInstitut d'astrophysique spatiale [IAS]
dc.contributor.authorARZOUMANIAN, D.
hal.structure.identifierIstituto di Astrofisica e Planetologia Spaziali - INAF [IAPS]
dc.contributor.authorBENEDETTINI, M.
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorCSENGERI, T.,
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorDIDELON, P.
hal.structure.identifierNRC Herzberg Institute of Astrophysics
dc.contributor.authorFRANCESCO, J. D.
hal.structure.identifierSchool of Physics and Astronomy [Cardiff]
dc.contributor.authorGRIFFIN, M.,
hal.structure.identifierJoint ALMA Observatory [JAO]
dc.contributor.authorHILL, T.
hal.structure.identifierZentrum für Astronomie der Universität Heidelberg [ZAH]
dc.contributor.authorKLESSEN, R. S.
hal.structure.identifierUniversität zu Köln = University of Cologne
dc.contributor.authorOSSENKOPF, V.
hal.structure.identifierIstituto di Astrofisica e Planetologia Spaziali - INAF [IAPS]
dc.contributor.authorPEZZUTO, S.
hal.structure.identifierOperations Department (ESAC)
dc.contributor.authorRIVERA-INGRAHAM, A.,
hal.structure.identifierIstituto di Astrofisica e Planetologia Spaziali - INAF [IAPS]
dc.contributor.authorSPINOGLIO, L.
hal.structure.identifierUniversity of Exeter
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorTREMBLIN, Pascal
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorZAVAGNO, Annie
dc.date.issued2015
dc.identifier.issn0035-8711
dc.description.abstractEnWe report the novel detection of complex high-column density tails in the probability distribution functions (PDFs) for three high-mass star-forming regions (CepOB3, MonR2, NGC6334), obtained from dust emission observed with Herschel. The low column density range can be fit with a lognormal distribution. A first power-law tail starts above an extinction (A$_v$) of ~6-14. It has a slope of $\alpha$ = 1.3$-$2 for the $\rho$ $\alpha$ $r^{-\alpha}$ profile for an equivalent density distribution (spherical or cylindrical geometry), and is thus consistent with free-fall gravitational collapse. Above A$_v$~40, 60, and 140, we detect an excess that can be fitted by a flatter power law tail with $\alpha$ > 2. It correlates with the central regions of the cloud (ridges/hubs) of size ~1 pc and densities above 10$^4$ cm$^{-3}$. This excess may be caused by physical processes that slow down collapse and reduce the flow of mass towards higher densities. Possible are: 1. rotation, which introduces an angular momentum barrier, 2. increasing optical depth and weaker cooling, 3. magnetic fields, 4. geometrical effects, and 5. protostellar feedback. The excess/second power-law tail is closely linked to high-mass star-formation though it does not imply a universal column density threshold for the formation of (high-mass) stars.
dc.description.sponsorshipVers une vision unifiée de la formation stellaire dans les galaxies : Origine de la structure filamentaire du milieu interstellaire, des cœurs pré-stellaires et des amas protostellaires vus avec Herschel
dc.language.isoen
dc.publisherOxford University Press (OUP): Policy P - Oxford Open Option A
dc.subject.enISM: clouds
dc.subject.endust extinction
dc.title.enDetection of two power-law tails in the probability distribution functions of massive GMCs
dc.typeArticle de revue
dc.identifier.doi10.1093/mnrasl/slv101
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.identifier.arxiv1507.08869
dc.description.sponsorshipEuropeToward a Complete View of Star Formation: The Origin of Molecular Clouds, Prestellar Cores, and Star Clusters
bordeaux.journalMonthly Notices of the Royal Astronomical Society
bordeaux.page41-45
bordeaux.volume453
bordeaux.peerReviewedoui
hal.identifierhal-01197448
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01197448v1
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