The [C ii] 158 Micron Emission from the Horsehead Nebula

Details The [C ii] 158 Micron Emission from the Horsehead Nebula The [C ii] 158 Micron Emission from the Horsehead Nebula

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...419..190z&link_type=abstract

Astrophysical Journal v.419, p.190

Astronomy and Astrophysics

Astronomy

22

Infrared: Interstellar: Lines, Ism: Individual Alphanumeric: Ic 434, Ism: Molecules

Scientific paper

We have mapped the [C II] 158 microns line and observed several rotational lines of CO, 13CO and CS toward selected positions in the Horsehead extinction region in IC 434. The observations show that the region has a gas density of about 104 cm-3 and an external UV flux 20-100 times the average interstellar UV field. Although this is a regime where the C+ emission varies rapidly with UV intensity, fine-structure line emission from gas with this range of physical conditions has not been investigated previously. Comparisons of our results with models of photodissociation regions show that existing plane-parallel photodissociation region models are in general agreement with the observed intensity. It is not necessary to invoke a clumpy structure in the boundary layer to explain the observations, but the overall geometry of the cloud is important in determining the distribution of C+ emission.

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