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The role of Galactic H II regions in the formation of filaments

hal.structure.identifierLaboratoire d'Astrophysique de Marseille [LAM]
hal.structure.identifierInstitut universitaire de France [IUF]
dc.contributor.authorZAVAGNO, Annie
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR_7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorANDRÉ, Ph.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR_7158 / UMR_E_9005 / UM_112)]
hal.structure.identifierLeibniz-Institut für Astrophysik Potsdam [AIP]
dc.contributor.authorSCHULLER, F.
hal.structure.identifierSchool of Physics and Astronomy [Cardiff]
dc.contributor.authorPERETTO, N.
hal.structure.identifierKagoshima University
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR_7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorSHIMAJIRI, Y.
hal.structure.identifierInstituto de Astrofísica e Ciências do Espaço [IASTRO]
dc.contributor.authorARZOUMANIAN, D.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorCSENGERI, T.
dc.contributor.authorFIGUEIRA, M.
hal.structure.identifierJodrell Bank Centre for Astrophysics [JBCA]
dc.contributor.authorFULLER, G. A.
hal.structure.identifierJeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston]
dc.contributor.authorKÖNYVES, V.
hal.structure.identifierAstrophysique Interprétation Modélisation [AIM (UMR_7158 / UMR_E_9005 / UM_112)]
dc.contributor.authorMEN’SHCHIKOV, A.
hal.structure.identifierInstituto de Astrofísica e Ciências do Espaço [IASTRO]
dc.contributor.authorPALMEIRIM, P.
hal.structure.identifierInstitut d'Astrophysique de Paris [IAP]
dc.contributor.authorROUSSEL, H.
hal.structure.identifierLaboratoire d'Astrophysique de Marseille [LAM]
dc.contributor.authorRUSSEIL, D.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
hal.structure.identifierUniversity Hospital of Cologne [Cologne]
dc.contributor.authorSCHNEIDER, N.
hal.structure.identifierLaboratoire d'Astrophysique de Marseille [LAM]
dc.contributor.authorZHANG, S.
dc.date.issued2020
dc.identifier.issn0004-6361
dc.description.abstractEnContext. Massive stars and their associated ionized (H II) regions could play a key role in the formation and evolution of filaments that host star formation. However, the properties of filaments that interact with H II regions are still poorly known.Aims. To investigate the impact of H II regions on the formation of filaments, we imaged the Galactic H II region RCW 120 and its surroundings where active star formation takes place and where the role of ionization feedback on the star formation process has already been studied.Methods. We used the large-format bolometer camera ArTéMiS on the APEX telescope and combined the high-resolution ArTéMiS data at 350 and 450 μm with Herschel-SPIRE/HOBYS data at 350 and 500 μm to ensure good sensitivity to a broad range of spatial scales. This allowed us to study the dense gas distribution around RCW 120 with a resolution of 8′′ or 0.05 pc at a distance of 1.34 kpc.Results. Our study allows us to trace the median radial intensity profile of the dense shell of RCW 120. This profile is asymmetric, indicating a clear compression from the H II region on the inner part of the shell. The profile is observed to be similarly asymmetric on both lateral sides of the shell, indicating a homogeneous compression over the surface. On the contrary, the profile analysis of a radial filament associated with the shell, but located outside of it, reveals a symmetric profile, suggesting that the compression from the ionized region is limited to the dense shell. The mean intensity profile of the internal part of the shell is well fitted by a Plummer-like profile with a deconvolved Gaussian full width at half maximum of 0.09 pc, as observed for filaments in low-mass star-forming regions.Conclusions. Using ArTéMiS data combined with Herschel-SPIRE data, we found evidence for compression from the inner part of the RCW 120 ionized region on the surrounding dense shell. This compression is accompanied with a significant (factor 5) increase of the local column density. This study suggests that compression exerted by H II regions may play a key role in the formation of filaments and may further act on their hosted star formation. ArTéMiS data also suggest that RCW 120 might be a 3D ring, rather than a spherical structure.
dc.description.sponsorshipGENeration et Evolution des Structures du milieu InterStellaire - ANR-16-CE92-0035
dc.description.sponsorshipVers une vision unifiée de la formation stellaire dans les galaxies : Origine de la structure filamentaire du milieu interstellaire, des cœurs pré-stellaires et des amas protostellaires vus avec Herschel
dc.description.sponsorshipARchitectures de bolomètres pour des TElescopes à grand champ de vue dans le domaine sub-MIllimétrique au Sol - ANR-05-BLAN-0215
dc.description.sponsorshipDes détecteurs pour Observer l'Univers
dc.language.isoen
dc.publisherEDP Sciences
dc.subject.enstars: formation
dc.subject.enH II regions
dc.subject.enISM: individual objects: RCW 120
dc.subject.ensubmillimeter: ISM
dc.title.enThe role of Galactic H II regions in the formation of filaments
dc.title.enHigh-resolution submilimeter imaging of RCW 120 with ArTéMiS
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/202037815
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]
dc.description.sponsorshipEuropeToward a Complete View of Star Formation: The Origin of Molecular Clouds, Prestellar Cores, and Star Clusters
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageA7
bordeaux.volume638
bordeaux.peerReviewedoui
hal.identifiercea-02654382
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//cea-02654382v1
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