2010A&A...521L..39K

Query : 2010A&A...521L..39K

2010A&A...521L..39K - Astronomy and Astrophysics, volume 521, L39-39 (2010/10-1)

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

KAMA M., DOMINIK C., MARET S., VAN DER TAK F., CAUX E., CECCARELLI C., FUENTE A., CRIMIER N., LORD S., BACMANN A., BAUDRY A., BELL T., BENEDETTINI M., BERGIN E.A., BLAKE G.A., BOOGERT A., BOTTINELLI S., CABRIT S., CASELLI P., CASTETS A., CERNICHARO J., CODELLA C., COMITO C., COUTENS A., DEMYK K., ENCRENAZ P., FALGARONE E., GERIN M., GOLDSMITH P.F., HELMICH F., HENNEBELLE P., HENNING T., HERBST E., HILY-BLANT P., JACQ T., KAHANE C., KLOTZ A., LANGER W., LEFLOCH B., LIS D., LORENZANI A., MELNICK G., NISINI B., PACHECO S., PAGANI L., PARISE B., PEARSON J., PHILLIPS T., SALEZ M., SARACENO P., SCHILKE P., SCHUSTER K., TIELENS X., VAN DER WIEL M.H.D., VASTEL C., VITI S., WAKELAM V., WALTERS A., WYROWSKI F., YORKE H., CAIS P., GUESTEN R., PHILIPP S., KLEIN T. and HELMICH F.

Abstract (from CDS):

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 961GHz cover a range in upper level energy of 40 to 540K. 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.

Abstract Copyright: ∼

Journal keyword(s): stars: formation - ISM: abundances - ISM: kinematics and dynamics - ISM: molecules

Simbad objects: 2

Full paper

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Number of rows : 2

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Mag U	Mag B	Mag V	Mag R	Mag I	Sp type	#ref 1850 - 2023	#notes
1	V* V2457 Ori	Or*	05 35 26.97000	-05 09 54.4644					18.858	~	148	0
2	2MASS J05352762-0509337	Y*O	05 35 27.622	-05 09 33.78						~	94	0

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