Ultraviolet-illuminated molecular cloud boundaries: Extended (C II) 158 micron emission toward L1630

Details Ultraviolet-illuminated molecular cloud boundaries: Extended (C II) 158 micron emission toward L1630 Ultraviolet-illuminated molecular cloud boundaries: Extended (C II) 158 micron emission toward L1630

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...436..203j&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-367X), vol. 436, no. 1, p. 203-215

Astronomy and Astrophysics

Astrophysics

32

Carbon, Galaxies, Molecular Clouds, Molecular Spectra, Ultraviolet Emission, Carbon Monoxide, Flux Density

Scientific paper

We have made a large-scale map of the 158 micrometers C(+) line toward the L1630/Orion B molecular cloud. The map covers a approximately 35 min x 45 min area which includes the NGC 2024 H II region, zeta Ori, the reflection nebula NGC 2023, and the Horsehead nebula. Emission in the (C II) line is very widespread. The line was detected at levels in excess of a few 10-4 ergs/sq cm/s/sr over almost the entire mapped region. Extended emission associated with the NGC 2024 H II region and its envelope accounts for more than half of the (C II) flux. Over this approximately 1.5 x 2.5 pc region, the amount of gas-phase carbon in the form of C(+) is comparable to the amount of carbon in CO. This result, together with the (C II) distribution, implies that (C II) emission arises on the surfaces of clumps throughout the cloud rather than in a single layer at the H II region boundary. Away from the H II region, most of the (C II) emission comes from the western edge of the L1630 cloud and probably results from excitation by external OB stars. The overall extent of the (C II) emission is comparable to that of millimeter molecular lines, but the distributions are different in detail. The difference in (C II) and molecular line distributions, in particular, the larger extent of the (C II) emission west of NGC 2024 implies large variations in the radio of the (C II) and CO J = 1 goes to 0 intensities. Models of photon-dominated regions can explain the relation between (C II) and CO intensities only if one considers the cloud edges and cloud interior separately. We propose a method for using (C II) and radio continuum emission to characterize the relationship between OB stars and photon-dominated regions.

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