Temperatures in the Orion molecular cloud as estimated from methyl cyanide observations

Details Temperatures in the Orion molecular cloud as estimated from methyl cyanide observations Temperatures in the Orion molecular cloud as estimated from methyl cyanide observations

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...136..243a&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 136, no. 2, July 1984, p. 243-249.

Astronomy and Astrophysics

Astrophysics

13

Astronomical Spectroscopy, Cyanides, Gas Temperature, Methyl Compounds, Molecular Clouds, Orion Nebula, Abundance, Acetonitrile, Gas Density, Radiative Transfer, Radio Spectra

Scientific paper

The J = 6→5 (K = 0-5) and J = 4→3 (K = 0-3) transitions of methyl cyanide (CH3CN) have been observed in Orion A. Because of the high dipole moment of CH3CN a thermal population distribution among its energy states does not usually exist in molecular clouds and the authors have found that neither a simple rotation diagram analysis nor the method of Hollis et al. (1981) is appropriate for determining kinetic temperatures. This has been verified by means of a statistical equilibrium analysis including 91 energy levels up to 200K. Using the statistical equilibrium analysis the authors estimate the kinetic temperatures in the Orion A hot core and compact ridge clouds to be 120±15K and ⪆110K, respectively. The Gaussian half power sizes of both emission regions appear to be ⪉35arcsec. The statistical equilibrium analysis also gives the column density and an estimate of the density of the regions.

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