White, Glenn J.; Richardson, K. J.; Avery, L. W. and Lesurf, J. C. G.
|DOI (Digital Object Identifier) Link:||http://dx.doi.org/10.1086/164031|
|Google Scholar:||Look up in Google Scholar|
A submillimeter wavelength spectroscopic study of the Orion molecular cloud has been made in the J = 4-3 HCN, HC13N, HCO+, HC13O+, and J = 7-6 CS molecular transitions. Densities of up to a few times 106 cm-3 are found coupled with high inferred brightness temperatures, indicating kinetic temperatures of 120 K. Evidence for lower densities in the surrounding ambient molecular cloud is presented along with maps of HCN and HCO+ emission. The maps indicate different spatial distributions in the two lines. The abundances of HCN and HCO+ in the plateau source are found to be enhanced relative to those in the surrounding molecular cloud, and there is a suggestion that a number of small-angular-diameter clumps may be present. The present observations do not confirm the previously reported detection of CO+ in the interstellar medium.
|Item Type:||Journal Article|
|Copyright Holders:||1986 The American Astronomical Society|
|Keywords:||formyl ions; hydrocyanic acid; molecular clouds; molecular spectroscopy; Orion nebula; submillimeter waves; abundance; brightness temperature; carbon monoxide|
|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:||10 Feb 2012 10:17|
|Last Modified:||18 Jan 2016 12:04|
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