Volume 407, Number 1, August III 2003
|Page(s)||237 - 248|
|Section||Interstellar and circumstellar matter|
|Published online||17 November 2003|
A molecular line survey of the candidate massive Class 0 protostar IRAS 23385+6053
Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK e-mail: firstname.lastname@example.org; email@example.com
Corresponding author: M. A. Thompson, firstname.lastname@example.org
Accepted: 21 May 2003
We have carried out a molecular line survey of the candidate massive protostar IRAS 23385+6053, covering a 27.2 GHz frequency range in the 330–360 GHz atmospheric window. We detected 27 lines originating from a total of 11 species. Over a third of the identified molecular lines are from the asymmetric top molecule methanol (CH3OH). We did not detect any emission from high-excitation lines or typical hot core tracers (e.g. CH3CN, HCOOCH3). We derive a rotation temperature and column density from the methanol emission and estimate lower limits to the beam-averaged column density of the remaining lines. Upper limits to the beam-averaged column density of selected species were determined from the non-detection of their rotation lines. We rule out the presence of a hot molecular core associated with IRAS 23385+6053 by a combination of the non-detection of CH3CN emission and a simple bolometric luminosity approach. The molecular inventory and chemistry of IRAS 23385+6053 are contrasted to that of more evolved massive star-forming regions and the abundances predicted by recent time-dependent chemical models. The physical and chemical nature of IRAS 23385+6053 is shown to be consistent with that immediately prior to the hot molecular core stage.
Key words: ISM: abundances / ISM: individual object: IRAS 23385+6053 / ISM: molecules / stars: formation
© ESO, 2003
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