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dc.contributor.author
Nony, T.
dc.contributor.author
Galván Madrid, R.
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Motte, F.
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Pouteau, Y.
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Cunningham, N.
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Louvet, F.
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Stutz, A. M.
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Lefloch, B.
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Bontemps, Sophie
dc.contributor.author
Brouillet, N.
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Ginsburg, A.
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Joncour, I.
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Herpin, F.
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Sanhueza, P.
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Csengeri, T.
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Towner, A. P. M.
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Bonfand, M.
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Fernandez Lopez, Manuel
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Baug, T.
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Bronfman, L.
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Busquets, Gabriel
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Di Francesco, J.
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Gusdorf, A.
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Lu, X.
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Olguin, F.
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Valeille-Manet, M.
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Whitworth, A. P.
dc.date.available
2023-12-01T16:20:40Z
dc.date.issued
2023-06
dc.identifier.citation
Nony, T.; Galván Madrid, R.; Motte, F.; Pouteau, Y.; Cunningham, N.; et al.; ALMA-IMF. V : prestellar and protostellar core populations in the W43 cloud complex; EDP Sciences; Astronomy and Astrophysics; 674; A75; 6-2023; 1-27
dc.identifier.issn
0004-6361
dc.identifier.uri
http://hdl.handle.net/11336/219065
dc.description.abstract
Context. The origin of the stellar initial mass function (IMF) and its relation with the core mass function (CMF) are actively debated issues with important implications in astrophysics. Recent observations in the W43 molecular complex of top-heavy CMFs, with an excess of high-mass cores compared to the canonical mass distribution, raise questions about our understanding of the star formation processes and their evolution in space and time.Aims: We aim to compare populations of protostellar and prestellar cores in three regions imaged in the ALMA-IMF Large Program.Methods: We created an homogeneous core catalogue in W43, combining a new core extraction in W43-MM1 with the catalogue of W43-MM2&MM3 presented in a previous work. Our detailed search for protostellar outflows enabled us to identify between 23 and 30 protostellar cores out of 127 cores in W43-MM1 and between 42 and 51 protostellar cores out of 205 cores in W43-MM2&MM3. Cores with neither outflows nor hot core emission are classified as prestellar candidates.Results: We found a similar fraction of cores which are protostellar in the two regions, about 35%. This fraction strongly varies in mass, from fpro ≃ 15-20% at low mass, between 0.8 and 3 M⊙ up to fpro ≃ 80% above 16 M⊙. Protostellar cores are found to be, on average, more massive and smaller in size than prestellar cores. Our analysis also revealed that the high-mass slope of the prestellar CMF in W43, α = -1.46-0.19+0.12, is consistent with the Salpeter slope, and thus the top-heavy form measured for the global CMF, α = −0.96 ± 0.09, is due to the protostellar core population.Conclusions: Our results could be explained by `clump-fed´ models in which cores grow in mass, especially during the protostellar phase, through inflow from their environment. The difference between the slopes of the prestellar and protostellar CMFs moreover implies that high-mass cores grow more in mass than low-mass cores.The CO(2-1) data cubes of W43-MM2 and W43-MM3, and full Tables F.1 and F.2 are available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (ftp://130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/674/A75
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
EDP Sciences
dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
stars: formation
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stars: massive
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stars: protostars
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ISM: clouds
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Astronomía
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Ciencias Físicas
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CIENCIAS NATURALES Y EXACTAS
dc.title
ALMA-IMF. V : prestellar and protostellar core populations in the W43 cloud complex
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2023-11-13T15:51:03Z
dc.journal.volume
674
dc.journal.number
A75
dc.journal.pagination
1-27
dc.journal.pais
Francia
dc.description.fil
Fil: Nony, T.. Universidad Autónoma de México. Instituto de Radioastronomía y Astrofísica ; México
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Fil: Galván Madrid, R.. Universidad Autónoma de México. Instituto de Radioastronomía y Astrofísica ; México
dc.description.fil
Fil: Motte, F.. Universite Grenoble Alpes; Suiza
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Fil: Pouteau, Y.. Universite Grenoble Alpes; Suiza
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Fil: Cunningham, N.. Universite Grenoble Alpes; Suiza
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Fil: Louvet, F.. Universite Grenoble Alpes; Suiza
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Fil: Stutz, A. M.. Universidad de Concepción; Chile
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Fil: Lefloch, B.. Universite Grenoble Alpes; Suiza
dc.description.fil
Fil: Bontemps, Sophie. Universite de Bordeaux; Francia
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Fil: Brouillet, N.. Universite de Bordeaux; Francia
dc.description.fil
Fil: Ginsburg, A.. University of Virginia; Estados Unidos
dc.description.fil
Fil: Joncour, I.. Universite de Bordeaux; Francia
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Fil: Herpin, F.. Universite de Bordeaux; Francia
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Fil: Sanhueza, P.. National Astronomical Observatory of Japan; Japón
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Fil: Csengeri, T.. Universite de Bordeaux; Francia
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Fil: Towner, A. P. M.. University of Virginia; Estados Unidos
dc.description.fil
Fil: Bonfand, M.. Universite de Bordeaux; Francia
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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: Baug, T.. Korea Astronomy And Space Science Institute; Corea del Sur
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Fil: Bronfman, L.. Universidad de Chile; Chile
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Fil: Busquets, Gabriel. Universidad de Barcelona; España
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Fil: Di Francesco, J.. Academia Sinica. Institute of Astronomy and Astrophysics; China
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Fil: Gusdorf, A.. Universite Paris-Saclay; Francia
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Fil: Lu, X.. Academia Sinica. Institute of Astronomy and Astrophysics; China
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Fil: Olguin, F.. National Tsing Hua University; China
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Fil: Valeille-Manet, M.. Universite de Bordeaux; Francia
dc.description.fil
Fil: Whitworth, A. P.. University of Virginia; Estados Unidos
dc.journal.title
Astronomy and Astrophysics
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/10.1051/0004-6361/202244762
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1051/0004-6361/202244762
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