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dc.contributor.authorMOLET, J.
dc.contributor.authorBROUILLET, N.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG]
dc.contributor.authorNONY, T.
hal.structure.identifierLaboratoire d'Etude du Rayonnement et de la Matière en Astrophysique [LERMA (UMR_8112)]
hal.structure.identifierAstrophysique
dc.contributor.authorGUSDORF, Antoine
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG]
hal.structure.identifierCommissariat à l'énergie atomique et aux énergies alternatives [CEA]
dc.contributor.authorMOTTE, F.
dc.contributor.authorDESPOIS, D.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorLOUVET, F.
dc.contributor.authorBONTEMPS, Sylvain
dc.contributor.authorHERPIN, Fabrice
dc.date.issued2019
dc.identifier.issn0004-6361
dc.description.abstractEnContext. High-mass analogues of low-mass prestellar cores are searched for to constrain the models of high-mass star formation. Several high-mass cores, at various evolutionary stages, have been recently identified towards the massive star-forming region W43-MM1 and amongst them a high-mass prestellar core candidate.Aims. We aim to characterise the chemistry in this high-mass prestellar core candidate, referred to as W43-MM1 core #6, and its environment.Methods. Using ALMA high-spatial resolution data of W43-MM1, we have studied the molecular content of core #6 and a neighbouring high-mass protostellar core, referred to as #3, which is similar in size and mass to core #6. We first subtracted the continuum emission using a method based on the density distribution of the intensities on each pixel. Then, from the distribution of detected molecules, we identified the molecules centred on the prestellar core candidate (core #6) and those associated to shocks related to outflows and filament formation. Then we constrained the column densities and temperatures of the molecules detected towards the two cores.Results. While core #3 appears to contain a hot core with a temperature of about 190 K, core #6 seems to have a lower temperature in the range from 20 to 90 K from a rotational diagram analysis. We have considered different source sizes for core #6 and the comparison of the abundances of the detected molecules towards the core with various interstellar sources shows that it is compatible with a core of size 1000 au with T = 20−90 K or a core of size 500 au with T ~ 80 K.Conclusions. Core #6 of W43-MM1 remains one of the best high-mass prestellar core candidates even if we cannot exclude that it is at the very beginning of the protostellar phase of high-mass star formation.
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enstars: formation
dc.subject.enstars: massive
dc.subject.enISM: abundances
dc.subject.enISM: molecules
dc.subject.enradio lines: ISM
dc.title.enMolecular analysis of a high-mass prestellar core candidate in W43-MM1
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201935497
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.identifier.arxiv1905.12463
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA132
bordeaux.volume626
bordeaux.peerReviewedoui
hal.identifierhal-02144700
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-02144700v1
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