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The earliest phases of high-mass star formation, as seen in NGC 6334 by Herschel-HOBYS

dc.contributor.authorTIGÉ, J.
hal.structure.identifierSciences pour l'environnement [SPE]
dc.contributor.authorMOTTE, F.
hal.structure.identifierLaboratoire d'Astrophysique de Marseille [LAM]
dc.contributor.authorRUSSEIL, D.
hal.structure.identifierLaboratoire d'Astrophysique de Marseille [LAM]
dc.contributor.authorZAVAGNO, Annie
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorHENNEMANN, M.
hal.structure.identifierLaboratory for Atmospheric and Space Physics [Boulder] [LASP]
dc.contributor.authorSCHNEIDER, N.
dc.contributor.authorHILL, T.
dc.contributor.authorLUONG, Q. Nguyen
hal.structure.identifierHerzberg Institute of Astrophysics
dc.contributor.authorDI FRANCESCO, J.
hal.structure.identifierFORMATION STELLAIRE 2017
dc.contributor.authorBONTEMPS, Sylvain
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorLOUVET, F.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorDIDELON, P.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorKONYVES, V.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorANDRÉ, Ph.
dc.contributor.authorLEULEU, G.
dc.contributor.authorBARDAGI, J.
dc.contributor.authorANDERSON, L. D.
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.
dc.contributor.authorBERNARD, J.
hal.structure.identifierIstituto di Astrofisica e Planetologia Spaziali - INAF [IAPS]
dc.contributor.authorELIA, D.
hal.structure.identifierCentro de Matemática e Aplicações Fundamentais [CMAF]
dc.contributor.authorFIGUEIRA, M.
dc.contributor.authorKIRK, J.
dc.contributor.authorMARTIN, P. G.
dc.contributor.authorMINIER, V.
hal.structure.identifierIstituto di Fisica dello Spazio Interplanetario [IFSI]
dc.contributor.authorMOLINARI, S.
dc.contributor.authorNONY, T.
dc.contributor.authorPERSI, P.
hal.structure.identifierFaculty of Informatics [Lugano]
dc.contributor.authorPEZZUTO, S.
dc.contributor.authorPOLYCHRONI, D.
hal.structure.identifierSchool of Physics and Astronomy [Cardiff]
dc.contributor.authorRAYNER, T.
dc.contributor.authorRIVERA-INGRAHAM, A.
hal.structure.identifierInstitut d'Astrophysique de Paris [IAP]
dc.contributor.authorROUSSEL, H.
dc.contributor.authorRYGL, K.
hal.structure.identifierAntarctic Research a European Network for Astrophysics [ARENA]
dc.contributor.authorSPINOGLIO, L.
hal.structure.identifierEngineering Department
dc.contributor.authorWHITE, G. J.
dc.date.issued2017
dc.identifier.issn0004-6361
dc.description.abstractEnAims. To constrain models of high-mass star formation, the Herschel-HOBYS key program aims at discovering massive dense cores (MDCs) able to host the high-mass analogs of low-mass prestellar cores, which have been searched for over the past decade. We here focus on NGC 6334, one of the best-studied HOBYS molecular cloud complexes.Methods. We used Herschel/PACS and SPIRE 70−500 μm images of the NGC 6334 complex complemented with (sub)millimeter and mid-infrared data. We built a complete procedure to extract ~0.1 pc dense cores with the getsources software, which simultaneously measures their far-infrared to millimeter fluxes. We carefully estimated the temperatures and masses of these dense cores from their spectral energy distributions (SEDs). We also identified the densest pc-scale cloud structures of NGC 6334, one 2 pc × 1 pc ridge and two 0.8 pc × 0.8 pc hubs, with volume-averaged densities of ~105 cm-3. Results. A cross-correlation with high-mass star formation signposts suggests a mass threshold of 75 M⊙ for MDCs in NGC 6334. MDCs have temperatures of 9.5−40 K, masses of 75−1000 M⊙, and densities of 1 × 105−7 × 107 cm-3. Their mid-infrared emission is used to separate 6 IR-bright and 10 IR-quiet protostellar MDCs while their 70 μm emission strength, with respect to fitted SEDs, helps identify 16 starless MDC candidates. The ability of the latter to host high-mass prestellar cores is investigated here and remains questionable. An increase in mass and density from the starless to the IR-quiet and IR-bright phases suggests that the protostars and MDCs simultaneously grow in mass. The statistical lifetimes of the high-mass prestellar and protostellar core phases, estimated to be 1−7 × 104 yr and at most 3 × 105 yr respectively, suggest a dynamical scenario of high-mass star formation.Conclusions. The present study provides good mass estimates for a statistically significant sample, covering the earliest phases of high-mass star formation. High-mass prestellar cores may not exist in NGC 6334, favoring a scenario presented here, which simultaneously forms clouds, ridges, MDCs, and high-mass protostars.
dc.description.sponsorshipEtoiles Proto-OB : recherche systématique dans notre Galaxie des cibles pour ALMA
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.endust
dc.subject.enextinction
dc.subject.enISM: clouds
dc.subject.enstars: formation
dc.subject.ensubmillimeter: ISM
dc.subject.enstars: protostars
dc.subject.enISM: individual objects: NGC 6334
dc.title.enThe earliest phases of high-mass star formation, as seen in NGC 6334 by Herschel-HOBYS
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201628989
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]
dc.identifier.arxiv1703.09839
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA77
bordeaux.volume602
bordeaux.peerReviewedoui
hal.identifierhal-01500414
hal.version1
hal.invitednon
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01500414v1
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