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29 March 2024
 
  » arxiv » 1008.2513

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The methanol lines and hot core of OMC2-FIR4, an intermediate-mass protostar, with Herschel-HIFI
M. Kama ; C. Dominik ; S. Maret ; F. van der Tak ; E. Caux ; C. Ceccarelli ; A. Fuente ; N. Crimier ; S. Lord ; A. Bacmann ; A. Baudry ; T. Bell ; M. Benedettini ; E.A. Bergin ; G.A. Blake ; A. Boogert ; S. Bottinelli ; S. Cabrit ; P. Caselli ; A. Castets ; J. Cernicharo ; C. Codella ; C. Comito ; A. Coutens ; K. Demyk ; P. Encrenaz ; E. Falgarone ; M. Gerin ; P.F. Goldsmith ; F. Helmich ; P. Hennebelle ; T. Henning ; E. Herbst ; P. Hily-Blant ; T. Jacq ; C. Kahane ; A. Klotz ; W. Langer ; B. Lefloch ; D. Lis ; A. Lorenzani ; G. Melnick ; B. Nisini ; S. Pacheco ; L. Pagani ; B. Parise ; J. Pearson ; T. Phillips ; M. Salez ; P. Saraceno ; P. Schilke ; K. Schuster ; A.G.G.M. Tielens ; M.H.D. van der Wiel ; C. Vastel ; S. Viti ; V. Wakelam ; A. Walters ; F. Wyrowski ; H. Yorke ; P. Cais ; R. Güsten ; S. Philipp ; T. Klein ;
Date 15 Aug 2010
AbstractIn contrast with numerous studies on the physical and chemical structure of low- and high-mass protostars, much less is known about their intermediate-mass counterparts, a class of objects that could help to elucidate the mechanisms of star formation on both ends of the mass range. We present the first results from a rich HIFI spectral dataset on an intermediate-mass protostar, OMC2-FIR4, obtained in the CHESS (Chemical HErschel SurveyS of star forming regions) key programme. The more than 100 methanol lines detected between 554 and 961 GHz cover a range in upper level energy of 40 to 540 K. Our physical interpretation focusses on the hot core, but likely the cold envelope and shocked regions also play a role in reality, because an analysis of the line profiles suggests the presence of multiple emission components. An upper limit of 10^-6 is placed on the methanol abundance in the hot core, using a population diagram, large-scale source model and other considerations. This value is consistent with abundances previously seen in low-mass hot cores. Furthermore, the highest energy lines at the highest frequencies display asymmetric profiles, which may arise from infall around the hot core.
Source arXiv, 1008.2513
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