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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.authorCSENGERI, T.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorBONTEMPS, S.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorBROUILLET, N.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG]
dc.contributor.authorMOTTE, F.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG]
dc.contributor.authorLOUVET, F.
hal.structure.identifierDepartment of Astronomy, University of Florida, PO Box 112055, USA
dc.contributor.authorGINSBURG, A.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG]
dc.contributor.authorCUNNINGHAM, N.
hal.structure.identifierInstituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia, Michoacán 58089, México
dc.contributor.authorGALVÁN-MADRID, R.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorHERPIN, F.
hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorWYROWSKI, F.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorVALEILLE-MANET, M.
hal.structure.identifierDepartamento de Astronomía, Universidad de Concepción, Casilla 160-C, 4030000 Concepción, Chile
dc.contributor.authorSTUTZ, A.
hal.structure.identifierHerzberg Astronomy and Astrophysics Research Centre, National Research Council of Canada, 5071 West Saanich Road, Victoria, BC V9E 2E7 Canada
dc.contributor.authorDI FRANCESCO, J.
hal.structure.identifierLaboratoire de physique de l'ENS - ENS Paris [LPENS]
dc.contributor.authorGUSDORF, A.
hal.structure.identifierInstituto Argentino de Radioastronomía (CCT-La Plata, CONICET; CICPBA), C.C. No. 5, 1894, Villa Elisa, Buenos Aires, Argentina
dc.contributor.authorFERNÁNDEZ-LÓPEZ, M.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorLEFLOCH, B.
hal.structure.identifierDepartamento de Astronomía, Universidad de Concepción, Casilla 160-C, 4030000 Concepción, Chile
dc.contributor.authorLIU, H-L.
hal.structure.identifierNational Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
dc.contributor.authorSANHUEZA, P.
hal.structure.identifierDepartamento de Astronomía, Universidad de Concepción, Casilla 160-C, 4030000 Concepción, Chile
dc.contributor.authorÁLVAREZ-GUTIÉRREZ, R.
hal.structure.identifierInstitute of Astronomy and Department of Physics, National Tsing Hua University, Hsinchu 30013, Taiwan
dc.contributor.authorOLGUIN, F.
hal.structure.identifierInstituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia, Michoacán 58089, México
dc.contributor.authorNONY, T.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG]
dc.contributor.authorLOPEZ-SEPULCRE, A.
hal.structure.identifierLaboratoire de physique de l'ENS - ENS Paris [LPENS]
dc.contributor.authorDELL’OVA, P.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG]
dc.contributor.authorPOUTEAU, Y.
hal.structure.identifierDepartment of Astronomy, University of Florida, PO Box 112055, USA
dc.contributor.authorJEFF, D.
hal.structure.identifierInstitute of Astronomy and Department of Physics, National Tsing Hua University, Hsinchu 30013, Taiwan
dc.contributor.authorCHEN, H.-R.
hal.structure.identifierLaboratoire de physique de l'ENS - ENS Paris [LPENS]
dc.contributor.authorARMANTE, M.
hal.structure.identifierUniversity of Arizona Department of Astronomy and Steward Observatory, 933 North Cherry Avenue, Tucson, AZ 85721, USA
dc.contributor.authorTOWNER, A.
hal.structure.identifierDepartamento de Astronomia, Universidad de Chile, Casilla 36-D, 1058, Santiago, Italy
dc.contributor.authorBRONFMAN, L.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorKESSLER, N.
dc.date.issued2024-07-09
dc.identifier.issn0004-6361
dc.description.abstractEnContext. The star formation process leads to an increased chemical complexity in the interstellar medium. Sites associated with high-mass star and cluster formation exhibit a so-called hot core phase, characterized by high temperatures and column densities of complex organic molecules. Aims. We aim to systematically search for and identify a sample of hot cores toward the 15 Galactic protoclusters of the ALMA-IMF Large Program and investigate their statistical properties. Methods. We built a comprehensive census of hot core candidates toward the ALMA-IMF protoclusters based on the detection of two CH 3 OCHO emission lines at 216.1 GHz. We used the source extraction algorithm GExt2D to identify peaks of methyl formate (CH 3 OCHO) emission, a complex species commonly observed toward sites of star formation. We performed a cross-matching with the catalog of thermal dust continuum sources from the ALMA-IMF 1.3 mm continuum data to infer their physical properties. Results. We built a catalog of 76 hot core candidates with masses ranging from ~0.2 M ⊙ to ~80 M ⊙ , of which 56 are new detections. A large majority of these objects, identified from methyl formate emission, are compact and rather circular, with deconvolved full width at half maximum (FWHM) sizes of ~2300 au on average. The central sources of two target fields show more extended, but still rather circular, methyl formate emission with deconvolved FWHM sizes of ~6700 au and 13 400 au. About 30% of our sample of methyl formate sources have core masses above 8 M ⊙ and range in size from ~1000 au to 13 400 au, which is in line with measurements of archetypical hot cores. The origin of the CH 3 OCHO emission toward the lower-mass cores may be explained as a mixture of contributions from shocks or may correspond to objects in a more evolved state (i.e., beyond the hot core stage). We find that the fraction of hot core candidates increases with the core mass, suggesting that the brightest dust cores are all in the hot core phase. Conclusions. Our results suggest that most of these compact methyl formate sources are readily explained by simple symmetric models, while collective effects from radiative heating and shocks from compact protoclusters are needed to explain the observed extended CH 3 OCHO emission. The large fraction of hot core candidates toward the most massive cores suggests that they rapidly enter the hot core phase and that feedback effects from the forming protostar(s) impact their environment on short timescales.
dc.language.isoen
dc.publisherEDP Sciences
dc.rights.urihttp://creativecommons.org/licenses/by/
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/202347856
dc.subject.halPlanète et Univers [physics]
dc.identifier.arxiv2402.15023
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA163
bordeaux.volume687
bordeaux.peerReviewedoui
hal.identifierhal-04783249
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-04783249v1
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