Afficher la notice abrégée

Filaments in the Lupus molecular clouds

hal.structure.identifierINAF - Osservatorio Astronomico di Roma [OAR]
dc.contributor.authorBENEDETTINI, M.
hal.structure.identifierINAF - Osservatorio Astronomico di Roma [OAR]
dc.contributor.authorSCHISANO, E.
hal.structure.identifierINAF - Osservatorio Astronomico di Roma [OAR]
dc.contributor.authorPEZZUTO, S.
hal.structure.identifierINAF - Osservatorio Astronomico di Roma [OAR]
dc.contributor.authorELIA, D.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR_7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorANDRÉ, P.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR_7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorKÖNYVES, V.
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorSCHNEIDER, N.
hal.structure.identifierUniversity of Exeter
hal.structure.identifierMaison de la Simulation [MDLS]
hal.structure.identifierUniversité de Versailles Saint-Quentin-en-Yvelines [UVSQ]
dc.contributor.authorTREMBLIN, Pascal
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR_7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorARZOUMANIAN, D.
hal.structure.identifierINAF - Osservatorio Astronomico di Roma [OAR]
dc.contributor.authorDI GIORGIO, A. M.
hal.structure.identifierUniversity of Victoria [Canada] [UVIC]
hal.structure.identifierNational Research Council of Canada [NRC]
dc.contributor.authorDI FRANCESCO, J.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR_7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorHILL, T.
hal.structure.identifierINAF - Osservatorio Astronomico di Roma [OAR]
dc.contributor.authorMOLINARI, S.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR_7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorMOTTE, F.
hal.structure.identifierNational Astronomical Observatory of Japan [NAOJ]
hal.structure.identifierCanadian Institute for Theoretical Astrophysics [CITA]
dc.contributor.authorNGUYEN-LUONG, Q.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR_7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorPALMEIRIM, P.
hal.structure.identifierInstitut de recherche en astrophysique et planétologie [IRAP]
dc.contributor.authorRIVERA-INGRAHAM, A.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR_7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorROY, A.
hal.structure.identifierINAF - Osservatorio Astronomico di Bologna [OABO]
dc.contributor.authorRYGL, K. L. J.
hal.structure.identifierINAF - Osservatorio Astronomico di Roma [OAR]
dc.contributor.authorSPINOGLIO, L.
hal.structure.identifierJeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston]
dc.contributor.authorWARD-THOMPSON, D.
hal.structure.identifierThe Rutherford Appleton Laboratory, Chilton, Didcot, Oxfordshire
hal.structure.identifierThe Open University [Milton Keynes] [OU]
dc.contributor.authorWHITE, G. J.
dc.date.issued2015
dc.identifier.issn0035-8711
dc.description.abstractEnWe have studied the filaments extracted from the column density maps of the nearby Lupus 1, 3, and 4 molecular clouds, derived from photometric maps observed with the Herschel satellite. Filaments in the Lupus clouds have quite low column densities, with a median value of ~ 1.5 × 10$^{21}$ cm$^{-2}$ and most have masses per unit length lower than the maximum critical value for radial gravitational collapse. Indeed, no evidence of filament contraction has been seen in the gas kinematics. We find that some filaments, that on average are thermally subcritical, contain dense cores that may eventually form stars. This is an indication that in the low column density regime, the critical condition for the formation of stars may be reached only locally and this condition is not a global property of the filament. Finally, in Lupus we find multiple observational evidences of the key role that the magnetic field plays in forming filaments, and determining their confinement and dynamical evolution.
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.enstars: formation
dc.subject.enISM: clouds
dc.title.enFilaments in the Lupus molecular clouds
dc.typeArticle de revue
dc.identifier.doi10.1093/mnras/stv1750
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.identifier.arxiv1507.08786
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.page2036-2049
bordeaux.volume453
bordeaux.issue2
bordeaux.peerReviewedoui
hal.identifierhal-01197451
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01197451v1
bordeaux.COinSctx_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.jtitle=Monthly%20Notices%20of%20the%20Royal%20Astronomical%20Society&rft.date=2015&rft.volume=453&rft.issue=2&rft.spage=2036-2049&rft.epage=2036-2049&rft.eissn=0035-8711&rft.issn=0035-8711&rft.au=BENEDETTINI,%20M.&SCHISANO,%20E.&PEZZUTO,%20S.&ELIA,%20D.&ANDR%C3%89,%20P.&rft.genre=article


Fichier(s) constituant ce document

FichiersTailleFormatVue

Il n'y a pas de fichiers associés à ce document.

Ce document figure dans la(les) collection(s) suivante(s)

Afficher la notice abrégée