The kinetic temperature and CH3CCH column density profiles in SGR B2, Orion, and DR 21

Details The kinetic temperature and CH3CCH column density profiles in SGR B2, Orion, and DR 21 The kinetic temperature and CH3CCH column density profiles in SGR B2, Orion, and DR 21

Sep 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...272..591c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 272, Sept. 15, 1983, p. 591-608.

Other

42

Interstellar Gas, Methyl Compounds, Molecular Clouds, Orion Nebula, Abundance, Acetonitrile, Acetylene, Gas Density, Gas Temperature, Molecular Energy Levels, Molecular Excitation, Molecular Rotation, Spectral Line Width

Scientific paper

Kinetic temperatures, T(kin), are presently estimated by means of a technique employing the intensities of the adjacent rotational transitions of symmetric top molecules, under the assumptions that the metastable levels are thermalized, and that the excitation temperature connecting the upper level of the observed transition to the lowest level in the K ladder is the same for the both adjacent transitions. The method is applied to observations of the J = 5-4 and J = 6-5 transitions of CH3CCH obtained at 1-arcmin intervals along a NS-EW cross that centered on Orion KL, Sgr B2, and Dr 21. The technique's application to CH3CN lines from the central positions of Sgr B2 and Orion produces T(kin) values that are in good agreement with other determinations. The fact that these lines are broader than those of CH3CCH is interpreted in terms of a model in which CH3CN emission is confined to small and warm core region while CH3CCH emission is dominated by a more extensive, almost isothermal and cooler halo region in Orion KL and Sgr B2.

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