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A new view of the Cygnus X region KOSMA 13 CO 2 1, 3 2, and 12 CO 3 2 imaging

dc.contributor.authorSCHNEIDER, N.
hal.structure.identifierLaboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorBONTEMPS, Sylvain
dc.contributor.authorSIMON, R.
dc.contributor.authorJAKOB, H.
dc.contributor.authorMOTTE, F.
dc.contributor.authorMILLER, M.
dc.contributor.authorKRAMER, C.
dc.contributor.authorSTUTZKI, J.
dc.date.issued2006
dc.identifier.issn0004-6361
dc.description.abstractEnContext: .The Cygnus X region is one of the richest star formation sites in the Galaxy. There is a long-standing discussion about whether the region is a chance superposition of several complexes along the line of sight or a single coherent complex at a distance of 1.5 to 2 kpc. Aims: . Combining a 13CO 2 to 1 survey taken with the KOSMA 3 m telescope with mid-IR images from MSX provides a way to improve our understanding of the spatial structure of the complex. The physical properties of the molecular gas can be derived in more detail as it was done in former studies. Methods: . Cygnus X has been mapped in 13CO J =2to1 (10.8 deg^2) at an angular resolution of 130'', as well as for smaller areas in 12CO and 13CO J = 3 to 2 (90''), using the KOSMA 3 m submm-telescope. Results: .We identified 91 clumps in 13CO 2 to 1 that have a typical excitation temperature of 10-30 K, an average density of 1.3×103 cm-3, radii of 1-8 pc, and masses of a few hundred to several ten thousand M_?. The main cloud complexes, the northern part (M≃2.8×10^5 M_?) including DR21 and W75N and the southern region (M≃4.5×10^5 M_?) with IC 1318 b/c and AFGL2591, show differences in their physical properties. The 13CO emission is closely associated with mid-IR emission seen with MSX. We find evidence that Cygnus OB2 and Cygnus OB9 are affecting the molecular material in Cygnus X. Conclusions: . Since essentially all molecular cloud complexes in Cygnus X form groups that are connected by molecular emission (visible in channel and position-velocity maps) and partly show evidence of interaction with UV radiation, we conclude that most of the objects seen in this region are located at the same distance, i.e., that of the OB2 cluster at 1.7 kpc, which is also consistent with the distances of other OB associations (OB9, OB1) in Cygnus X.
dc.language.isoen
dc.publisherEDP Sciences
dc.rights.urihttp://creativecommons.org/licenses/by/
dc.subject.ensubmillimeter
dc.subject.enISM: individual objects: Cygnus X region
dc.subject.enISM: structure
dc.subject.enISM: clouds
dc.title.enA new view of the Cygnus X region KOSMA 13 CO 2 1, 3 2, and 12 CO 3 2 imaging
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361:20065088
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Cosmologie et astrophysique extra-galactique [astro-ph.CO]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.page855-871
bordeaux.volume458
bordeaux.peerReviewedoui
hal.identifierhal-00129250
hal.version1
hal.popularnon
hal.audienceNon spécifiée
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00129250v1
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