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ALMA-IMF

dc.contributor.authorÁLVAREZ-GUTIÉRREZ, R.
dc.contributor.authorSTUTZ, A.
dc.contributor.authorSANDOVAL-GARRIDO, N.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG]
dc.contributor.authorLOUVET, F.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG]
dc.contributor.authorMOTTE, F.
dc.contributor.authorGALVÁN-MADRID, R.
dc.contributor.authorCUNNINGHAM, N.
dc.contributor.authorSANHUEZA, P.
hal.structure.identifierDepartments of Astronomy and Chemistry, University of Virginia, Charlottesville, VA 22904, USA
dc.contributor.authorBONFAND, M.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorBONTEMPS, S.
hal.structure.identifierLaboratoire de physique de l'ENS - ENS Paris [LPENS]
dc.contributor.authorGUSDORF, A.
dc.contributor.authorGINSBURG, A.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorCSENGERI, T.
dc.contributor.authorREYES, S.
dc.contributor.authorSALINAS, J.
hal.structure.identifierS. N. Bose National Centre for Basic Sciences, Sector-III, Salt Lake, Kolkata 700106, India
dc.contributor.authorBAUG, T.
hal.structure.identifierAstronomy Department, Universidad de Chile, Camino El Observa- torio 1515, Las Condes, Santiago, Chile
dc.contributor.authorBRONFMAN, L.
hal.structure.identifierDepartament de Física Quàntica i Astrofísica (FQA), Universitat de Barcelona (UB ), Martí i Franquès 1, 08028 Barcelona, Catalonia, Spain
dc.contributor.authorBUSQUET, G.
dc.contributor.authorDÍAZ-GONZÁLEZ, D.
dc.contributor.authorFERNANDEZ-LOPEZ, M.
dc.contributor.authorGUZMÁN, A.
dc.contributor.authorKOLEY, A.
hal.structure.identifierSchool of Physics and Astronomy, Yunnan University
dc.contributor.authorLIU, H.-L.
dc.contributor.authorOLGUIN, F.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorVALEILLE-MANET, M.
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorWYROWSKI, F.
dc.date.issued2024-09-04
dc.identifier.issn0004-6361
dc.description.abstractEnThe ALMA-IMF Large Program provides multi-tracer observations of 15 Galactic massive protoclusters at a matched sensitivity and spatial resolution. We focus on the dense gas kinematics of the G353.41 protocluster traced by N 2 H + (1−0), with a spatial resolution of ~0.02 pc. G353.41, at a distance of ~2kpc, is embedded in a larger-scale (~8 pc) filament and has a mass of ~2.5 × 10 3 M ⊙ within 1.3 × 1.3 pc 2 . We extracted the N 2 H + (1−0) isolated line component and decomposed it by fitting up to three Gaussian velocity components. This allows us to identify velocity structures that are either muddled or impossible to identify in the traditional position-velocity diagram. We identify multiple velocity gradients on large (~1 pc) and small scales (~0.2pc). We find good agreement between the N 2 H + velocities and the previously reported DCN core velocities, suggesting that cores are kinematically coupled with the dense gas in which they form. We have measured nine converging “V-shaped” velocity gradients (VGs) (~20 km s −1 pc −1 ) that are well resolved (sizes ~0.1 pc), mostly located in filaments, which are sometimes associated with cores near their point of convergence. We interpret these V-shapes as inflowing gas feeding the regions near cores (the immediate sites of star formation). We estimated the timescales associated with V-shapes as VG −1 , and we interpret them as inflow timescales. The average inflow timescale is ~67 kyr, or about twice the free-fall time of cores in the same area (~33 kyr) but substantially shorter than protostar lifetime estimates (~0.5 Myr). We derived mass accretion rates in the range of (0.35–8.77) × 10 −4 M ⊙ yr −1 . This feeding might lead to further filament collapse and the formation of new cores. We suggest that the protocluster is collapsing on large scales, but the velocity signature of collapse is slow compared to pure free-fall. Thus, these data are consistent with a comparatively slow global protocluster contraction under gravity, and faster core formation within, suggesting the formation of multiple generations of stars over the protocluster’s lifetime.
dc.language.isoen
dc.publisherEDP Sciences
dc.rights.urihttp://creativecommons.org/licenses/by/
dc.title.enALMA-IMF
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/202450321
dc.subject.halPlanète et Univers [physics]
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA74
bordeaux.volume689
bordeaux.peerReviewedoui
hal.identifierhal-04783179
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-04783179v1
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