White, Glenn J. and Sandell, Goeran
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The spatial distributions of the 3P1-3P0 atomic fine structure of carbon (CI), the CO J=4-3,the CO J=2→1 transitions of CO, 13CO, C18O and C17O and the 790 μm continuum emission have been mapped towards the central region of the Orion molecular cloud (OMC1 cloud), and the Bright Bar ionisation front. The CO data are analysed in a consistent way, allowing the inter isotopomeric abundance ratios to be studied over a wide range of extinction values. The 13CO lines are optically thick; the 13CO abundance being enhanced because of strong isotopic fractionation near the Bright Bar, but less convincingly in the OMC1 cloud. The fractionation occurs mostly in the less opaque regions where the 13CO column density N(13CO) may be enhanced by up to one order of magnitude, relative to the more shielded parts. No isotope selective enhancement of the other CO isotopomers was seen; C18O may in fact show a slight depletion in more exposed material. The C18O and C17O lines are optically thin, and correlated with the 790 μm dust continuum emission. The CI emission comes from hot optically thin gas; the abundance ratios of CI/CO are typically 0.05-0.3, with the larger ratios towards the northern section of the Orion ridge. The CI abundance ratios remain high along the edge of the Bright Bar which is adjacent to the HII region (and the Trapezium cluster which excites it), but decrease in the dense shielded material behind the Bar.
|Item Type:||Journal Article|
|Copyright Holders:||1996 European Southern Observatory|
|Keywords:||atoms; molecules; Orion cloud; Orion bar; abundances; radio lines|
|Academic Unit/Department:||Science > Physical Sciences
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||G. J. White|
|Date Deposited:||23 Mar 2012 09:11|
|Last Modified:||26 Feb 2016 05:41|
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