Volume 407, Number 2, August IV 2003
|Page(s)||589 - 607|
|Section||Interstellar and circumstellar matter|
|Published online||17 November 2003|
A spectral survey of the Orion Nebula from 455–507 GHz
Centre for Astrophysics & Planetary Science, University of Kent, Canterbury, Kent CT2 7NR, UK
2 Stockholm Observatory, 133 36 Saltsjöbaden, Sweden
3 Astrophysics Group, The Cavendish Laboratory, University of Cambridge, Madingley Road, Cambridge CB3 OHE, UK
4 Institute for Physical Chemistry, University of Basel, Klingelbergstrasse 80, 4056 Basel, Switzerland
5 Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK
6 National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, Tokyo 181-8588, Japan
7 Department of Physics, Queen Mary & Westfield College, University of London, Mile End Road, London E1 4NS, UK
Corresponding author: Glenn J. White, email@example.com
Accepted: 22 May 2003
The results of a submillimetre wavelength spectral line survey between 455.1–507.4 GHz of the Orion-KL hot cloud core are reported. A total of 254 lines were detected to a main beam brightness temperature sensitivity ~ 1–3 K. The detected lines are identified as being associated with 30 different molecular species or their isotopomeric variants. The strongest line detected was the J = 4–3 transition of the CO molecule. Apart from abundant diatomic rotors such as CO and CS, the spectrum is dominated by SO, SO2 and CH3OH and large organic molecules such as (CH3)2O, CH3CN, C2H3CN, C2H5CN and HCOOCH3 which make up ~72% of the total number of lines; unidentified lines ~13%; and other lines the remaining ~15% of the total. Rotational temperatures and column densities derived using standard rotation diagram analysis techniques were found to range from 70–300 K, and 1014–10 cm respectively.
Key words: molecules / star formation / molecular cloud
© ESO, 2003
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