A Caltech Library Service

The methanol lines and hot core of OMC2-FIR4, an intermediate-mass protostar, with Herschel/HIFI

Kama, M. and Lord, S. and Bell, T. and Blake, G. A. and Boogert, A. and Lis, D. and Phillips, T. G. (2010) The methanol lines and hot core of OMC2-FIR4, an intermediate-mass protostar, with Herschel/HIFI. Astronomy and Astrophysics, 521 . L39. ISSN 0004-6361. doi:10.1051/0004-6361/201015118.

PDF - Published Version
See Usage Policy.


Use this Persistent URL to link to this item:


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 Survey 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.

Item Type:Article
Related URLs:
URLURL TypeDescription
Blake, G. A.0000-0003-0787-1610
Boogert, A.0000-0001-9344-0096
Lis, D.0000-0002-0500-4700
Additional Information:© 2010 ESO. Received 31 May 2010; Accepted 29 July 2010; Published online 01 October 2010. Herschel is an ESA space observatory with science instruments provided by European-led principal Investigator consortia and with important participation from NASA. The authors are grateful to the referee, Dr. Tim van Kempen, for constructive comments leading to a significant improvement of the paper, and to Rens Waters for helpful discussions. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri- INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio AstronŮmico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology – MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University – Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC, and we are deeply grateful to everyone involved in the designing, building, and exploitation of this fantastic instrument. HCSS, HSpot, and HIPE are joint developments by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS, and SPIRE consortia. M.Kama gratefully acknowledges support from the Netherlands Organisation for Scientific Research (NWO) grant number 021.002.081 and the Leids Kerkhoven-Bosscha Fonds, and thanks SRON Groningen for hosting the HIFI ICC volunteers.
Funding AgencyGrant Number
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)021.002.081
Leids Kerkhoven-Bosscha FondsUNSPECIFIED
Subject Keywords:stars: formation; ISM: abundances; ISM: kinematics and dynamics; ISM: molecules
Record Number:CaltechAUTHORS:20110110-112346500
Persistent URL:
Official Citation: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, X. 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 and F. Helmich A&A 521 L39 (2010) DOI: 10.1051/0004-6361/201015118
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:21665
Deposited On:10 Jan 2011 22:09
Last Modified:09 Nov 2021 15:59

Repository Staff Only: item control page