Atomic carbon and CO isotope emission in the vicinity of the Orion Bar.

Details Atomic carbon and CO isotope emission in the vicinity of the Orion Bar. Atomic carbon and CO isotope emission in the vicinity of the Orion Bar.

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...297..567t&link_type=abstract

Astronomy and Astrophysics, v.297, p.567

Astronomy and Astrophysics

Astrophysics

46

Ism: Atoms, Ism: Clouds, Ism: Individual Objects: Orion, Radio Lines: Ism

Scientific paper

We present observations of the ^3^P_1_-^3^P_0_ fine structure transition of atomic carbon, as well as of the J=2-1 transition of ^13^CO and C^18^O toward the Orion Bar, the south-eastern rim of the cavity carved out in the Orion molecular cloud by the Hii region surrounding the Trapezium stars. The Orion Bar is a dense region illuminated by an intense flux of UV photons, i.e. a photodissociation or photon-dominated region (PDR). The observed Ci intensity agrees with models of uniform-density edge-on PDRs, which predict a spatially stratified morphology for the ionized, neutral, and molecular components. Our observations, however, show a surprisingly good spatial correlation between Ci and ^13^CO. The bright neutral carbon and ^13^CO emission from the Bar is superposed on a broad plateau of extended emission. The origin of this extended distribution may lie in the particular geometry of the region, which gives rise to face-on PDRs associated with the back and front walls of the cavity. Because of their weak emission, we infer that these face-on PDRs must be clumpy with a low beam filling factor (~30-40%) in contrast to the Bar which has been shown to have a filling factor of ~1 for radiation from the ionizing stars.

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