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Self-absorption in [CII], ^12CO, and HI in RCW120. Building up a geometrical and physical model of the region

dc.contributor.authorKABANOVIC, S.
hal.structure.identifierLaboratory for Atmospheric and Space Physics [Boulder] [LASP]
dc.contributor.authorSCHNEIDER, N.
hal.structure.identifierUniversität zu Köln = University of Cologne
dc.contributor.authorOSSENKOPF-OKADA, V.
dc.contributor.authorFALASCA, F.
hal.structure.identifierDivision for Submm Technologies
dc.contributor.authorGÜSTEN, R.
hal.structure.identifierPhysikalisches Institut [Köln]
dc.contributor.authorSTUTZKI, J.
dc.contributor.authorSIMON, R.
hal.structure.identifierInstituto de RadioAstronomía Milimétrica [IRAM]
dc.contributor.authorBUCHBENDER, C.
dc.contributor.authorANDERSON, L.
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorBONNE, L.
dc.contributor.authorGUEVARA, C.
hal.structure.identifierUniversity of Michigan [Ann Arbor]
dc.contributor.authorHIGGINS, R.
hal.structure.identifierAustralia Telescope National Facility
dc.contributor.authorKORIBALSKI, B.
hal.structure.identifierWest Virginia University [Morgantown]
dc.contributor.authorLUISI, M.
dc.contributor.authorMERTENS, M.
dc.contributor.authorOKADA, Y.
hal.structure.identifierPhysikalisches Institut [Köln]
dc.contributor.authorRÖLLIG, M.
dc.contributor.authorSEIFRIED, D.
dc.contributor.authorTIWARI, M.
hal.structure.identifierMax Planck Institute for Radio Astronomy
dc.contributor.authorWYROWSKI, F.
hal.structure.identifierLaboratoire d'Astrophysique de Marseille [LAM]
dc.contributor.authorZAVAGNO, Annie
dc.contributor.authorTIELENS, A.~g.~g.~m.
dc.date.issued2021
dc.description.abstractEnRevealing the 3D dynamics of HII regions and their associated molecular clouds is important for understanding the longstanding problem as to how stellar feedback affects the density structure and kinematics of the interstellar medium. We employed observations of the HII region RCW 120 in [CII], observed within the SOFIA legacy program FEEDBACK, and the ^12CO and ^13CO (3\to2) lines, obtained with APEX. In addition we used HI data from the Southern Galactic Plane Survey. Two radiative transfer models were used to fit the observed data. A line profile analysis with the 1D non-LTE radiative transfer code SimLine proves that the CO emission cannot stem from a spherically symmetric molecular cloud configuration. With a two-layer multicomponent model, we then quantified the amount of warm background and cold foreground gas. There is a deficit of CO emission along the line-of-sight toward the center of the HII region which indicates that the HII region is associated with a flattened molecular cloud. Self-absorption in the CO line may hide signatures of infalling and expanding molecular gas. The [CII] emission arises from an expanding [CII] bubble and from the PDRs. A significant part of [CII] emission is absorbed in a cool (\raisebox-0.5ex~60-100 K), low-density (<500 cm^-3) atomic foreground layer with a thickness of a few parsec. We propose that the RCW 120 HII region formed in a flattened molecular cloud and is now bursting out of its parental cloud. The compressed surrounding molecular layer formed a torus around the spherically expanding HII bubble. This scenario can possibly be generalized for other HII bubbles and would explain the observed ``flat'' structure of molecular clouds associated with HII bubbles. We suggest that the [CII] absorption observed in many star-forming regions is at least partly caused by low-density, cool, HI-envelopes surrounding the molecular clouds.
dc.language.isoen
dc.subject.enAstrophysics - Astrophysics of Galaxies
dc.title.enSelf-absorption in [CII], ^12CO, and HI in RCW120. Building up a geometrical and physical model of the region
dc.typeArticle de revue
dc.identifier.doi10.48550/arXiv.2112.11336
dc.subject.halPlanète et Univers [physics]
bordeaux.journalArXiv e-prints
bordeaux.pagearXiv:2112.11336
bordeaux.peerReviewedoui
hal.identifierhal-03561791
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-03561791v1
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