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Massive clumps in W43-main: Structure formation in an extensively shocked molecular cloud

hal.structure.identifierMax-Planck-Institut für Radioastronomie [MPIFR]
dc.contributor.authorWYROWSKI, F.
hal.structure.identifierNanjing Southeast University [SEU]
dc.contributor.authorLIU, H.
hal.structure.identifierMax-Planck-Institut für Extraterrestrische Physik [MPE]
dc.contributor.authorSIPILÄ, O.
dc.contributor.authorIZQUIERDO, A.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorCSENGERI, T.
hal.structure.identifierDepartment of Astronomy, University of Florida, P.O. Box 112055, Gainesville, FL 32611, USA
dc.contributor.authorGINSBURG, A.
hal.structure.identifierCenter for Astrochemical Studies [CAS@MPE]
dc.contributor.authorSPEZZANO, S.
hal.structure.identifierINAF - Osservatorio Astronomico di Cagliari [OAC]
dc.contributor.authorLEURINI, S.
hal.structure.identifierMax Planck Institute for Extraterrestrial Physics [MPE]
dc.contributor.authorCASELLI, P.
hal.structure.identifierMax Planck Institute for Radio Astronomy
dc.contributor.authorMENTEN, K.
dc.date.accessioned2024-11-22T03:11:09Z
dc.date.available2024-11-22T03:11:09Z
dc.date.issued2024-05-15
dc.identifier.issn0004-6361
dc.identifier.urihttps://oskar-bordeaux.fr/handle/20.500.12278/203416
dc.description.abstractEnAims . W43-main is a massive molecular complex undergoing starburst activities, located at the interaction of the Scutum arm and the Galactic bar. We aim to investigate the gas dynamics, in particular, the prevailing shock signatures from cloud to clump scales. We also look to assess the impact of shocks on the formation of dense gas and early-stage cores in OB cluster formation processes. Methods . We carried out NOEMA and IRAM-30 m observations at 3 mm towards five molecular gas clumps in W43 main located within large-scale interacting gas components. We used CH 3 CCH and H 2 CS lines to trace the extended gas temperature and CH 3 OH lines to probe the volume density of the dense gas components (≳10 5 cm −3 ). We adopted multiple tracers that are sensitive to different gas density regimes to reflect the global gas motions. The density enhancements constrained by CH 3 OH and a population of NH 2 D cores are correlated (in the spatial and velocity domains) with SiO emission, which is a prominent indicator of shock processing in molecular clouds. Results . The emission of SiO (2–1) is extensive across the region (~4 pc) and it is contained within a low-velocity regime, hinting at a large-scale origin for the shocks. Position-velocity maps of multiple tracers show systematic spatio-kinematic offsets supporting the cloud-cloud collision-merging scenario. We identified an additional extended velocity component in the CCH emission, which coincides with one of the velocity components of the larger scale 13 CO (2−1) emission, likely representing an outer, less-dense gas layer in the cloud merging process. We find that the ‘V-shaped’, asymmetric SiO wings are tightly correlated with localised gas density enhancements, which is direct evidence of dense gas formation and accumulation in shocks. The dense gas that is formed in this way may facilitate the accretion of the embedded, massive pre-stellar and protostellar cores. We resolved two categories of NH 2 D cores: those exhibiting only subsonic to transonic velocity dispersions and those with an additional supersonic velocity dispersion. The centroid velocities of the latter cores are correlated with the shock front seen via SiO. The kinematics of the ~0.1 pc NH 2 D cores are heavily imprinted by shock activities and may represent a population of early-stage cores forming around the shock interface.
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enMassive clumps in W43-main: Structure formation in an extensively shocked molecular cloud
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/202348959
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique galactique [astro-ph.GA]
dc.identifier.arxiv2401.17192
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA101
bordeaux.volume685
bordeaux.hal.laboratoriesLaboratoire d'Astrophysique de Bordeaux (LAB) - UMR 5804*
bordeaux.institutionUniversité de Bordeaux
bordeaux.institutionCNRS
bordeaux.peerReviewedoui
hal.identifierhal-04795867
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-04795867v1
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