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Class 0 Protostars in the Perseus Molecular Cloud: A Correlation Between the Youngest Protostars and the Dense Gas Distribution

dc.contributor.authorSADAVOY, S. I.
hal.structure.identifierHerzberg Institute of Astrophysics
dc.contributor.authorDI FRANCESCO, J.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorANDRE, Ph.
hal.structure.identifierIstituto di Fisica dello Spazio Interplanetario [IFSI]
dc.contributor.authorPEZZUTO, S.
dc.contributor.authorBERNARD, J. -P.
hal.structure.identifierSan Pedro de Atacama Celestial Explorations [SPACE]
dc.contributor.authorMAURY, A.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorMEN'SHCHIKOV, A.
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.authorNGUYEN-LUONG, Q.
hal.structure.identifierFORMATION STELLAIRE 2014
dc.contributor.authorSCHNEIDER, N.
dc.contributor.authorARZOUMANIAN, D.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG ]
dc.contributor.authorBENEDETTINI, M.
hal.structure.identifierFORMATION STELLAIRE 2014
dc.contributor.authorBONTEMPS, Sylvain
dc.contributor.authorELIA, D.
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.authorKONYVES, V.
hal.structure.identifierGroupe d'Etudes des Matériaux Hétérogènes [GEMH]
dc.contributor.authorLOUVET, François
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.
hal.structure.identifierEngineering Department
dc.contributor.authorWHITE, G. J.
dc.date.created2014-04-28
dc.date.issued2014
dc.identifier.issn2041-8205
dc.description.abstractEnWe use PACS and SPIRE continuum data at 160 um, 250 um, 350 um, and 500 um from the Herschel Gould Belt Survey to sample seven clumps in Perseus: B1, B1-E, B5, IC348, L1448, L1455, and NGC1333. Additionally, we identify and characterize the embedded Class 0 protostars using detections of compact Herschel sources at 70 um as well as archival Spitzer catalogues and SCUBA 850 um photometric data. We identify 28 candidate Class 0 protostars, four of which are newly discovered sources not identified with Spitzer. We find that the star formation efficiency of clumps, as traced by Class 0 protostars, correlates strongly with the flatness of their respective column density distributions at high values. This correlation suggests that the fraction of high column density material in a clump reflects only its youngest protostellar population rather than its entire source population. We propose that feedback from either the formation or evolution of protostars changes the local density structure of clumps.
dc.language.isoen
dc.publisherBristol : IOP Publishing
dc.title.enClass 0 Protostars in the Perseus Molecular Cloud: A Correlation Between the Youngest Protostars and the Dense Gas Distribution
dc.typeArticle de revue
dc.identifier.doi10.1088/2041-8205/787/2/L18
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.identifier.arxiv1404.7142
bordeaux.journalThe Astrophysical journal letters
bordeaux.pageL18
bordeaux.volume787
bordeaux.issue2
bordeaux.peerReviewedoui
hal.identifierhal-00987362
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00987362v1
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