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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 | Abstract: | In 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 | Services: | Forum | Review | PDF | Favorites |
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