[C I] 809 GHz Imaging of the NGC 6334 Complex

• Published in: Publications of the Astronomical Society of Japan
• Main Authors: Kim, Sungeun, Narayanan, Desika
• Format: Article in Journal/Newspaper
• Language: English
• Published: Oxford University Press (OUP) 2006
• Subjects: Space and Planetary Science; Astronomy and Astrophysics; Antarctic; Antarc*
• Online Access: http://dx.doi.org/10.1093/pasj/58.4.753; https://academic.oup.com/pasj/article-pdf/58/4/753/9714458/pasj58-0753.pdf

We present Antarctic Submillimeter Telescope and Remote Observatory (AST/RO) observations of submillimeter emissions from the NGC 6334 complex for both the $^{12}[\mathrm{C {I}}] \; {{3\atop} \mathrm{P}}_2 \rightarrow {{3\atop} \mathrm{P}}_1$ fine-structure line of atomic carbon and the ${{12\atop} \mathrm{CO}} J = 4 \rightarrow 3$ rotational transition of CO. We detected strong $^{12}[\mathrm{C {I}}] \; {{3\atop} \mathrm{P}}_2 \rightarrow {{3\atop} \mathrm{P}}_1$ emission from the entire star-forming NGC 6334 complex, and present maps of $^{12}[\mathrm{C {I}}] \; {{3\atop} \mathrm{P}}_2 \rightarrow {{3\atop} \mathrm{P}}_1$ emission and ${{12\atop} \mathrm{CO}} J = 4 \rightarrow 3$ emission. Comparing these maps with archival ASCA data, we show that, to the south of NGC 6334, the [C I] emissions are likely to be associated with strong X-ray emissions from the FIR sources. However, the calculation using the X-ray dissociation region model shows that the majority of the [C I] emission can not arise from X-ray dissociation of the cloud. Alternatively, far-ultraviolet radiation produced in the photodissociation regions is expected to contribute to dissociate the carbon monoxide in the NGC 6334 complex.