Onsala high spatial resolution observations of HCN, HCO/+/, and their isotopes in Orion A

Details Onsala high spatial resolution observations of HCN, HCO/+/, and their isotopes in Orion A Onsala high spatial resolution observations of HCN, HCO/+/, and their isotopes in Orion A

Jan 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...243l..41r&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 243, Jan. 1, 1981, p. L41-L45.

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26

Abundance, Emission Spectra, Hydrocyanic Acid, Hydrogen Clouds, Interstellar Matter, Molecular Ions, Orion Nebula, Carbon Isotopes, Gas Density, Interstellar Masers, Molecular Excitation

Scientific paper

The distributions of H(C-12)N, H(C-13)N, and H(C-12)O(+) are mapped with 20-arcsec spacing. H(C-15)N and H(C-13)O(+) are observed toward the map center. The physical properties of the Orion A extended ridge and of the much smaller HCN plateau cloud (angular extension considerably less than that of the 43-arcsec beam) are estimated on the basis of Gaussian decompositions of the various spectra, combined with cloud modeling. It is found that the HCN and HCO(+) abundances have the same order of magnitude in the ridge, whereas the former is more than 10 times larger in the plateau. The mean H(C-12)N/H(C-13)N density and the excitation temperature ratios are estimated; as expected, nearly the same ratio, H(C-12)N/H(C-13)N approximating 30, is found in the plateau and in the ridge clouds. The H(C-12)O(+)/H(C-13)O(+) ratio is put at roughly 30 in the ridge clouds. It is found that the ridge emission exhibits a fairly sharp velocity shift from approximately 8 km/sec in the SW to approximately 10 km/sec in the NE; this is thought to be caused by a transition from one ridge cloud to another. This twin cloud effect is seen as probably more pronounced in the case of H(C-15)N.

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