Further observations of rotationally excited far infrared OH16 and OH18 emission in Orion-KL: Tighter constraints on the nature of the emitting region

Details Further observations of rotationally excited far infrared OH16 and OH18 emission in Orion-KL: Tighter constraints on the nature of the emitting region Further observations of rotationally excited far infrared OH16 and OH18 emission in Orion-KL: Tighter constraints on the nature of the emitting region

Jul 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989stin...9014156m&link_type=abstract

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Computer Science

Excitation, Far Infrared Radiation, Hydroxyl Emission, Orion Nebula, Transition Probabilities, Emission Spectra, Energy Spectra, Flux (Rate), Flux Density, Galactic Clusters, Ground State, Line Spectra

Scientific paper

The Orion-KL region, within 1 arc minute, is observed. The rotational cross ladder (53.351 microns) and rotational ground state (120.1719 microns) transitions are studied. It is shown that these lines exhibit a P-Cygni profile and unambiguously show that the OH gas is expanding out from the central BN-KL infrared cluster. The OH-16 rotational ground state transition (119.234 microns) is velocity resolved and it is found that its intrinsic full width at half maximum is 75 km/s. The line fluxes and line profiles are modeled and it is shown that no single temperature and density component can reproduce the data. Rather, the best fit to the data requires emission from three main components of the gas: post shocked gas with the profiles of temperature, density, and OH abundance; a high density component to the cool post shocked region; and the plateau region.

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