Other
Scientific paper
Dec 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...189.2102k&link_type=abstract
American Astronomical Society, 189th AAS Meeting, #21.02; Bulletin of the American Astronomical Society, Vol. 28, p.1302
Other
3
Scientific paper
We have imaged the [O I] 63 mu m line around 5 FIR and radio continuum sources in the southern massive star formation region NGC 6334. We find evidence for [O I] absorption toward the FIR continuum source NGC 6334 V. This is the first instance in which the [O I] 63 mu m line has been observed in absorption against a continuum source. From the strength of the absorption, we calculate the column density of atomic oxygen to be N(O(0)~) 5.8+/-2.4*E(18) cm(-2) , which corresponds to a hydrogen column density of N(H)~ 1.2+/-0.5 *E(22) cm(-2) . This is more than an order of magnitude lower than the molecular column density derived from CO excitation models: N(H_2)~ 1.3*E(23) cm(-2) . We suggest that only a small fraction of the oxygen in the absorbing, foreground material, 5-10%, is in atomic form. The [O I] 63 mu m line is found in emission toward the other four sources observed: NGC 6334 A, C, D and E. Based on the [O I] 63 mu m data in combination with previously observed [O I] 146 mu m, [C II] 158 mu m, FIR and CO data, the best fits of single-component photodissociation region (PDR) models imply densities of n ~ 10(4) cm(-3) and UV field strengths of G_0 ~ 10(4) for NGC 6334 C, D and E. However, neither single- nor two-component PDR models can explain the anomalously faint [O I] 63 mu m intensity toward NGC 6334 A or NGC 6334 V. We suggest that the low [O I] 63 mu m intensity from NGC 6334 A is due to self-absorption. These results suggest that the 63 mu m [O I] line may commonly be absorbed by cold molecular gas, and its use as a PDR diagnostic is therefore problematic.
Jackson James M.
Kraemer Karl
Lane Adair P.
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