[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: Text
• Language: English
• Published: Oxford University Press 2006
• Subjects: Papers; Antarctic; Antarc*
• Online Access: http://pasj.oxfordjournals.org/cgi/content/short/58/4/753; https://doi.org/10.1093/pasj/58.4.753

We present Antarctic Submillimeter Telescope and Remote Observatory (AST/RO) observations of submillimeter emissions from the NGC 6334 complex for both the <f>$^{12}[\mathrm{C {I}}] \; {{3\atop} \mathrm{P}}_2 \rightarrow {{3\atop} \mathrm{P}}_1$</f> fine-structure line of atomic carbon and the <f>${{12\atop} \mathrm{CO}} J = 4 \rightarrow 3$</f> rotational transition of CO. We detected strong <f>$^{12}[\mathrm{C {I}}] \; {{3\atop} \mathrm{P}}_2 \rightarrow {{3\atop} \mathrm{P}}_1$</f> emission from the entire star-forming NGC 6334 complex, and present maps of <f>$^{12}[\mathrm{C {I}}] \; {{3\atop} \mathrm{P}}_2 \rightarrow {{3\atop} \mathrm{P}}_1$</f> emission and <f>${{12\atop} \mathrm{CO}} J = 4 \rightarrow 3$</f> 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.