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Discovery of warm and dense molecular gas surrounding the ring nebula G79.29+0.46

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dc.contributor.author Rizzo Caminos, José Ricardo
dc.contributor.author Jiménez-Esteban, F. M.
dc.contributor.author Ortiz, E.
dc.date.accessioned 2016-07-26T18:05:53Z
dc.date.available 2016-07-26T18:05:53Z
dc.date.issued 2008
dc.identifier.citation Rizzo, J. R., Jiménez-Esteban, F. M., & Ortiz, E. (2008). Discovery of warm and dense molecular gas surrounding the ring nebula G79. 29+ 0.46. The Astrophysical Journal, 681(1), 355. spa
dc.identifier.issn 0004637X
dc.identifier.issn 15384357
dc.identifier.uri http://hdl.handle.net/11268/5474
dc.description.abstract We present for the first time the detection of mid-J CO line emission in the outskirts of an evolved massive star, which indicates the presence of warm and/or high-density molecular gas. Aiming to learn about the interplay between evolved massive stars and their surroundings, we have carried out CO J = 2→ 1, J = 3→ 2, and 13↑CO J = 2→ 1 line observations in a 4' × 4' field around the ring nebula G79.29+0.46, which is illuminated by a strong LBV star candidate. The whole field shows extended predominant emission in both CO and 13↑CO J = 2→ 1 lines, which probably comes from the large cloud which contains the star-forming region DR 15. When this large-scale emission is removed, minor-scale features become evident, particularly in the CO J = 3→ 2 line, strikingly coincident with the ring nebula. The high critical density of CO J = 3→ 2 (some 10↑4 cm↑−3) gives additional support for the association with the massive star, since high-density molecular gas has more chances to survive in such a harsh environment. This structure may have been produced by the cumulative effect of a strong steady wind in the LBV stage or earlier, which has compressed the surviving parent molecular cloud. In addition, immersed within this CO feature, we have also discovered a higher density clump (at least several ~10↑5 cm↑−3), unresolved by the telescope and probably having a higher kinetic temperature. Toward the clump, the presence of a jump of 14-16 km s↑−1 in the gas velocity may indicate the existence of a shock front. This clump may have been created by at least one mass eruption, 10↑3-10↑4 yr ago. Thus, this work shows that not all the molecular gas is destroyed during massive star evolution, and consequently we are dealing with a new laboratory where one can learn about the mass-loss phenomena associated to the brief LBV stage. spa
dc.description.sponsorship SIN FINANCIACIÓN spa
dc.language.iso eng spa
dc.rights Reconocimiento-NoComercial-CompartirIgual 3.0
dc.rights.uri http://creativecommons.org/licenses/by-nc-sa/3.0/es/
dc.title Discovery of warm and dense molecular gas surrounding the ring nebula G79.29+0.46 spa
dc.type article spa
dc.description.impact 6.331 JCR (2008) Q1, 6/48 Astronomy & astrophysics spa
dc.rights.accessRights openAccess spa
dc.subject.uem Dióxido de carbono-Aspectos ambientales spa
dc.subject.unesco Astrofísica spa
dc.description.filiation UEM spa
dc.peerreviewed Si spa


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