ALMA-IMF: V. Prestellar and protostellar core populations in the W43 cloud complex
Por:
Nony T., Galván-Madrid R., Motte F., Pouteau Y., Cunningham N., Louvet F., Stutz A.M., Lefloch B., Bontemps S., Brouillet N., Ginsburg A., Joncour I., Herpin F., Sanhueza P., Csengeri T., Towner A.P.M., Bonfand M., Fernández-López M., Baug T., Bronfman L., Busquet G., Di Francesco J., Gusdorf A., Lu X., Olguin F., Valeille-Manet M., Whitworth A.P.
Publicada:
1 ene 2023
Resumen:
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, ? =-1.46-0.19+0.12, is consistent with the Salpeter slope, and thus the top-heavy form measured for the global CMF, ? = 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. © 2023 EDP Sciences. All rights reserved.
Filiaciones:
Nony T.:
Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia, Michoacán, 58089, Mexico
Galván-Madrid R.:
Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia, Michoacán, 58089, Mexico
Motte F.:
Univ. Grenoble Alpes, CNRS, IPAG, Grenoble, 38000, France
Pouteau Y.:
Univ. Grenoble Alpes, CNRS, IPAG, Grenoble, 38000, France
Cunningham N.:
Univ. Grenoble Alpes, CNRS, IPAG, Grenoble, 38000, France
Louvet F.:
Univ. Grenoble Alpes, CNRS, IPAG, Grenoble, 38000, France
Departamento de Astronomia, Universidad de Chile, Casilla 36-D, Santiago, Chile
Stutz A.M.:
Departamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile
Lefloch B.:
Univ. Grenoble Alpes, CNRS, IPAG, Grenoble, 38000, France
Bontemps S.:
Laboratoire d'Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, Allée Geoffroy Saint-Hilaire, Pessac, 33615, France
Brouillet N.:
Laboratoire d'Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, Allée Geoffroy Saint-Hilaire, Pessac, 33615, France
Ginsburg A.:
Department of Astronomy, University of Florida, PO Box 112055, Gainesville, FL 32611-2055, United States
Joncour I.:
Univ. Grenoble Alpes, CNRS, IPAG, Grenoble, 38000, France
Herpin F.:
Laboratoire d'Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, Allée Geoffroy Saint-Hilaire, Pessac, 33615, France
Sanhueza P.:
National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan
Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies), 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan
Csengeri T.:
Laboratoire d'Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, Allée Geoffroy Saint-Hilaire, Pessac, 33615, France
Towner A.P.M.:
Department of Astronomy, University of Florida, PO Box 112055, Gainesville, FL 32611-2055, United States
Bonfand M.:
Laboratoire d'Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, Allée Geoffroy Saint-Hilaire, Pessac, 33615, France
Department of Astronomy, University of Virginia, Charlottesville, VA 22904, United States
Fernández-López M.:
Instituto Argentino de Radioastronomía (CCT-La Plata CONICET
Baug T.:
S. N. Bose National Centre for Basic Sciences, Block JD, Sector III, Salt Lake, Kolkata, 700106, India
Bronfman L.:
Departamento de Astronomia, Universidad de Chile, Casilla 36-D, Santiago, Chile
Busquet G.:
Departament de Física Quàntica i Astrofísica (FQA), Universitat de Barcelona (UB, c. Martí i Franquès, 1, Barcelona, 08028, Spain
Institut de Ciències Del Cosmos (ICCUB), Universitat de Barcelona (UB), c. Martí i Franquès, 1, Barcelona, 08028, Spain
Institut D'Estudis Espacials de Catalunya (IEEC), c. Gran Capità 2-4, Barcelona, 08034, Spain
Di Francesco J.:
Herzberg Astronomy and Astrophysics Research Centre, National Research Council of Canada, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada
Gusdorf A.:
Laboratoire de Physique de L'Acole Normale Supérieure, ENS, Université PSL, CNRS, Sorbonne Université, Université Paris Cité, Paris, 75005, France
Observatoire de Paris, PSL University, Sorbonne Université, LERMA, Paris, 75014, France
Lu X.:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai, 200030, China
Olguin F.:
Institute of Astronomy and Department of Physics, National Tsing Hua University, Hsinchu, 30013, Taiwan
Valeille-Manet M.:
Laboratoire d'Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, Allée Geoffroy Saint-Hilaire, Pessac, 33615, France
Whitworth A.P.:
School of Physics and Astronomy, Cardiff University, Queen's Buildings, The Parade, Cardiff, CF24 3AA, United Kingdom
Department of Astronomy, University of Virginia, Charlottesville, VA 22904, United States
hybrid, Green Submitted, Hybrid Gold
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