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dc.contributor.author
Motte, F.
dc.contributor.author
Bontemps, S.
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Csengeri, T.
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Pouteau, Y.
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Louvet, F.
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Stutz, A.M.
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Cunningham, N.
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López Sepulcre, A.
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Brouillet, N.
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Galván-Madrid, R.
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Ginsburg, A.
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Maud, L.
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Men'shchikov, A.
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Nakamura, F.
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Nony, T.
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Sanhueza, P.
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Álvarez-Gutiérrez, R.H.
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Armante, M.
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Baug, T.
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Bonfand, M.
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Busquet, G.
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Chapillon, E.
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Díaz González, D.
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Fernandez Lopez, Manuel
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Tatematsu, K.
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Thomasson, B.
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Walker, D.
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Wu, B.
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Whitworth, A. P.
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Wyrowski, F.
dc.date.available
2023-10-26T16:13:49Z
dc.date.issued
2022-06
dc.identifier.citation
Motte, F.; Bontemps, S.; Csengeri, T.; Pouteau, Y.; Louvet, F.; et al.; ALMA-IMF: I. Investigating the origin of stellar masses: Introduction to the Large Program and first results; EDP Sciences; Astronomy and Astrophysics; 662; 6-2022; 1-27
dc.identifier.issn
0004-6361
dc.identifier.uri
http://hdl.handle.net/11336/216072
dc.description.abstract
Aims. Thanks to the high angular resolution, sensitivity, image fidelity, and frequency coverage of ALMA, we aim to improve our understanding of star formation. One of the breakthroughs expected from ALMA, which is the basis of our Cycle 5 ALMA-IMF Large Program, is the question of the origin of the initial mass function (IMF) of stars. Here we present the ALMA-IMF protocluster selection, first results, and scientific prospects. Methods. ALMA-IMF imaged a total noncontiguous area of ~53 pc2, covering extreme, nearby protoclusters of the Milky Way. We observed 15 massive (2.5 '33 - 103 M'), nearby (2'5.5 kpc) protoclusters that were selected to span relevant early protocluster evolutionary stages. Our 1.3 and 3 mm observations provide continuum images that are homogeneously sensitive to point-like cores with masses of ~0.2 M' and ~0.6 M', respectively, with a matched spatial resolution of ~2000 au across the sample at both wavelengths. Moreover, with the broad spectral coverage provided by ALMA, we detect lines that probe the ionized and molecular gas, as well as complex molecules. Taken together, these data probe the protocluster structure, kinematics, chemistry, and feedback over scales from clouds to filaments to cores. Results. We classify ALMA-IMF protoclusters as Young (six protoclusters), Intermediate (five protoclusters), or Evolved (four proto-clusters) based on the amount of dense gas in the cloud that has potentially been impacted by H II region(s). The ALMA-IMF catalog contains ~700 cores that span a mass range of ~0.15 M' to ~250 M' at a typical size of ~2100 au. We show that this core sample has no significant distance bias and can be used to build core mass functions (CMFs) at similar physical scales. Significant gas motions, which we highlight here in the G353.41 region, are traced down to core scales and can be used to look for inflowing gas streamers and to quantify the impact of the possible associated core mass growth on the shape of the CMF with time. Our first analysis does not reveal any significant evolution of the matter concentration from clouds to cores (i.e., from 1 pc to 0.01 pc scales) or from the youngest to more evolved protoclusters, indicating that cloud dynamical evolution and stellar feedback have for the moment only had a slight effect on the structure of high-density gas in our sample. Furthermore, the first-look analysis of the line richness toward bright cores indicates that the survey encompasses several tens of hot cores, of which we highlight the most massive in the G351.77 cloud. Their homogeneous characterization can be used to constrain the emerging molecular complexity in protostars of high to intermediate masses. Conclusions. The ALMA-IMF Large Program is uniquely designed to transform our understanding of the IMF origin, taking the effects of cloud characteristics and evolution into account. It will provide the community with an unprecedented database with a high legacy value for protocluster clouds, filaments, cores, hot cores, outflows, inflows, and stellar clusters studies.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
EDP Sciences
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dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
EVOLUTION
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H II REGIONS
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ISM: CLOUDS
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MASS FUNCTION
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STARS: FORMATION
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STARS: LUMINOSITY FUNCTION
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STARS: PROTOSTARS
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Astronomía
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Ciencias Físicas
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CIENCIAS NATURALES Y EXACTAS
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dc.title
ALMA-IMF: I. Investigating the origin of stellar masses: Introduction to the Large Program and first results
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2023-09-25T14:52:36Z
dc.journal.volume
662
dc.journal.pagination
1-27
dc.journal.pais
Francia
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dc.journal.ciudad
Paris
dc.description.fil
Fil: Motte, F.. Universite Grenoble Alpes; Francia
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Fil: Bontemps, S.. Universite de Bordeaux; Francia
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Fil: Csengeri, T.. Universite de Bordeaux; Francia
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Fil: Pouteau, Y.. Universite Grenoble Alpes; Francia
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Fil: Louvet, F.. Universidad de Chile; Chile. Universite Grenoble Alpes; Francia. Universite Paris-Saclay;
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Fil: Stutz, A.M.. Universidad de Concepción; Chile. Max Planck Institute For Astronomy; Alemania
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Fil: Cunningham, N.. Universite Grenoble Alpes; Francia
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Fil: López Sepulcre, A.. Universite Grenoble Alpes; Francia. Iram Institut de Radioastronomie Millimétrique; Francia
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Fil: Brouillet, N.. Universite de Bordeaux; Francia
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Fil: Galván-Madrid, R.. Instituto de Radioastronomía y Astrofísica; México
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Fil: Ginsburg, A.. University of Florida; Estados Unidos
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Fil: Maud, L.. European Southern Observatory Chile; Chile
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Fil: Men'shchikov, A.. Universite Paris-Saclay;
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Fil: Nakamura, F.. National Institutes Of Natural Sciences. National Astronomical Observatory Of Japan; Japón. The Graduate University For Advanced Studies; Japón
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Fil: Nony, T.. Instituto de Radioastronomía y Astrofísica; México
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Fil: Sanhueza, P.. The Graduate University For Advanced Studies; Japón. National Institutes Of Natural Sciences. National Astronomical Observatory Of Japan; Japón
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Fil: Álvarez-Gutiérrez, R.H.. Universidad de Concepción; Chile
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Fil: Armante, M.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia. Université Pierre et Marie Curie; Francia
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Fil: Baug, T.. S. N. Bose National Centre For Basic Sciences; India
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Fil: Bonfand, M.. Universite de Bordeaux; Francia
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Fil: Busquet, G.. Instituto de Estudios Espaciales de Cataluña; España. Universite Grenoble Alpes; Francia. Consejo Superior de Investigaciones Científicas; España
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Fil: Chapillon, E.. Universite de Bordeaux; Francia. Institut de Radioastronomie Millimétrique; Francia
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Fil: Díaz González, D.. Instituto de Radioastronomía y Astrofísica; México
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Fil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
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Fil: Tatematsu, K.. National Institutes Of Natural Sciences. National Astronomical Observatory Of Japan; Japón
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Fil: Thomasson, B.. Universite Grenoble Alpes; Francia
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Fil: Walker, D.. University of Connecticut; Estados Unidos
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Fil: Wu, B.. National Institutes Of Natural Sciences. National Astronomical Observatory Of Japan; Japón. Nvidia; Estados Unidos
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Fil: Whitworth, A. P.. Cardiff University; Reino Unido
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Fil: Wyrowski, F.. Max Planck Institute For Radio Astronomy; Alemania
dc.journal.title
Astronomy and Astrophysics
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dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1051/0004-6361/202141677
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2022/06/aa41677-21/aa41677-21.html
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