Molecular and Atomic Gas in the NGC 6334 Star Forming Region

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Session 26 -- Molecular Cloud Structure and Energetics
Oral presentation, Wednesday, January 12, 10:15-11:45, Crystal Forum Room (Crystal City Marriott)

[26.06] Molecular and Atomic Gas in the NGC 6334 Star Forming Region

K. E. Kraemer (Boston University), J. M. Jackson (Boston University), A. Lane (Harvard-Smithsonian Center for Astrophysics)

The NGC6334 molecular cloud complex presents a unique opportunity to examine the effects of massive star formation on the surrounding interstellar medium. Because it contains at least six distinct star forming sites, global factors such as global magnetic fields and elemental abundances are the same from site to site. Only local factors such as the mass, age, and UV field of the individual stars. We have mapped NGC 6334 in the CO and $^{13}$CO (J$=2\to 1$), and CS (J$=5\to 4$) lines with the CSO. The line ratios vary considerably at the various star forming sites within the cloud. We also have imaged the region in the far-infrared using the FIFI spectrometer on the KAO, in the [C II] 158 $\mu$, [O I] 63 $\mu$, and [O I] 145 $\mu$ lines. The ionized carbon to oxygen line ratios also vary from site to site. We have fit gray body models to IRAS HIRES images to determine the dust temperature at each site. We discuss the effects of the different stellar types of the newly formed massive stars on the molecular, atomic and ionized gas surrounding them.

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