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ALMA-IMF XVIII: The assembly of a star cluster: Dense N$_2$H$^+$ (1-0) kinematics in the massive G351.77 protocluster

hal.structure.identifierDepartamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile
dc.contributor.authorSANDOVAL-GARRIDO, N.
hal.structure.identifierDepartamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile
dc.contributor.authorSTUTZ, A.
hal.structure.identifierDepartamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile
dc.contributor.authorÁLVAREZ-GUTIÉRREZ, R.
hal.structure.identifierInstituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia, Michoacán 58089, México
dc.contributor.authorGALVÁN-MADRID, R.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG]
dc.contributor.authorMOTTE, F.
hal.structure.identifierDepartment of Astronomy, University of Florida, P.O. Box 112055, Gainesville, FL 32611
dc.contributor.authorGINSBURG, A.
hal.structure.identifierSKA Observatory, Jodrell Bank, Lower Withington, Macclesfield, SK11 9FT, United Kingdom
dc.contributor.authorCUNNINGHAM, N.
hal.structure.identifierDepartamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile
dc.contributor.authorREYES-REYES, S.
hal.structure.identifierEuropean Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching, Germany
dc.contributor.authorREDAELLI, E.
hal.structure.identifierDepartments of Astronomy and Chemistry, University of Virginia, Charlottesville, VA 22904, USA
dc.contributor.authorBONFAND, M.
hal.structure.identifierDepartamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile
dc.contributor.authorSALINAS, J.
hal.structure.identifierDepartamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile
dc.contributor.authorKOLEY, A.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorBRAINE, J.
hal.structure.identifierAstronomy Department, Universidad de Chile, Casilla 36-D, 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.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorCSENGERI, T.
dc.contributor.authorDI FRANCESCO, J.
hal.structure.identifierInstituto Argentino de Radioastronomía (CCT-La Plata, CONICET; UNLP; CICPBA), C.C. No. 5, 1894, Villa Elisa, Buenos Aires, Ar- gentin
dc.contributor.authorFERNÁNDEZ-LÓPEZ, M.
hal.structure.identifierChinese Academy of Sciences South America Center for Astron- omy, National Astronomical Observatories, CAS, Beijing 100101, China
dc.contributor.authorGARCIA, P.
hal.structure.identifierLaboratoire de physique de l'ENS - ENS Paris [LPENS]
dc.contributor.authorGUSDORF, A.
dc.contributor.authorLIU, H. -L.
hal.structure.identifierDepartment of Earth and Planetary Sciences, Institute of Science Tokyo, Meguro, Tokyo, 152-8551, Japan
dc.contributor.authorSANHUEZA, P.
dc.date2024
dc.date.issued2024
dc.identifier.issn0004-6361
dc.description.abstractEnALMA-IMF observed 15 massive protoclusters capturing multiple spectral lines and the continuum emission. We focus on the G351.77 protocluster ($\sim$ 2500 M$_{\odot}$, estimated from single-dish continuum observations) located at 2 kpc. We trace the dense gas emission and kinematics with N$_2$H$^+$ (1-0) at $\sim$ 4 kau resolution. We estimate an N$_2$H$^+$ relative abundance $\sim (1.7 \pm 0.5) \times 10^{-10}$. We decompose the N$_2$H$^+$ emission into up to two velocity components, highlighting the kinematic complexity in the dense gas. By examining the position-velocity (PV) diagrams on small scales, we observe clear inflow signatures (V-shapes) associated with dense cores. The most prominent V-shape has a mass inflow rate of $\sim 9.8 \times 10^{-4}$ M$_{\odot}$ yr$^{-1}$ and a short timescale of $\sim$ 15.6 kyr. We also observe V-shapes without associated cores. This suggests both that cores or centers of accretion exist below the 1.3 mm detection limit, and that the V-shapes may be viable tracers of very early accretion and star formation on $\sim$ 4 kau scales. The large-scale PV diagram shows that the protocluster is separated into 2 principal velocity structures. Combined with smaller scale DCN and H$_2$CO emission, we propose a scenario of larger scale slow contraction with rotation in the center based on simple toy models. This scenario leads the suggestion of outside-in evolution of the protocluster as it collapses. The gas depletion times implied by the V-shapes are short ($\sim$ 0.3 Myr), requiring either very fast cluster formation, and/or continuous mass feeding of the protocluster. The latter is possible via the Mother Filament G351.77 is forming out of. The similarities in the properties of G351.77 and the recently published work in G353.41 indicate that many of the physical conditions inferred via the ALMA-IMF N$_2$H$^+$ observations may be generic to protoclusters.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enAstrophysics of Galaxies (astro-ph.GA)
dc.subject.enFOS: Physical sciences
dc.title.enALMA-IMF XVIII: The assembly of a star cluster: Dense N$_2$H$^+$ (1-0) kinematics in the massive G351.77 protocluster
dc.typeArticle de revue
dc.identifier.doi10.48550/arXiv.2410.09843
dc.subject.halPlanète et Univers [physics]
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.peerReviewedoui
hal.identifierhal-04779898
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-04779898v1
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