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Large Scale Structure and Turbulence: The Mopra G333 Survey

Published online by Cambridge University Press:  04 October 2008

C. Kramer ,
S. Aalto ,
R. Simon ,
M. Cunningham ,
N. Lo ,
C. Kramer ,
I. Bains ,
P. Jones ,
M. Burton  and
E. Muller
...Show all authors
M. Cunningham
Affiliation:
School of Physics, University of New South Wales Sydney, Australia
N. Lo
Affiliation:
School of Physics, University of New South Wales Sydney, Australia
C. Kramer
Affiliation:
KOSMA. I. Physikalisches Institut, Universität zu Köln, Germany
I. Bains
Affiliation:
Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Australia
P. Jones
Affiliation:
School of Physics, University of New South Wales Sydney, Australia
M. Burton
Affiliation:
School of Physics, University of New South Wales Sydney, Australia
E. Muller
Affiliation:
Australia Telescope National Facility, CSIRO, Australia
V. Ossenkopf
Affiliation:
KOSMA. I. Physikalisches Institut, Universität zu Köln, Germany
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Abstract

We have used the new broadband capabilities of the Mopra telescope to map the distribution of 26 different molecular transitions in an approximately 1 degree square region of the southern Galactic plane (the G333/RCW106 giant molecular cloud complex). The aim is to addresss observationally some of the key questions about the dynamical processes surrounding massive star formation (e.g. massive stellar winds and large-scale galactic flows) and their relative importance in regulating the star formation process. These dynamical processes help drive the turbulent motions, which are ubiquitous in giant molecular clouds (GMCs). The multi-molecular line nature of this survey is what distinguishes it from similar surveys and is crucial for gaining a clear picture of the energetics and dynamics of the gas. Investigating and understanding the chemistry of this region is a necessary part of the project if the molecular line observations are to be interpreted physically.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 31: Far-Infrared Workshop 2007 , 2008 , pp. 9 - 14
Copyright
© EAS, EDP Sciences, 2008

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References

Bains, I., et al., 2006, MNRAS, 367, 1609 CrossRef
Elmegreen, B.G., & Scalo, J., 2004, ARA&A, 42, 211 CrossRef
Hasegawa, T.I., & Kwok, S., 2001, ApJ, 562, 824 CrossRef
Klein, C., et al., 2003, RevMexAA, 15, 92; Larson 2003, Rep. Prog. Phys., 66, 1651
Ladd, N., Purcell, C., Wong, T., & Robertson, S., 2005, PASA, 22, 62 CrossRef
Lo, N., Cunningham, M., Bains, I., Burton, M.G., & Garay, G., 2007, MNRAS, 381, L30 CrossRef
Lockman, F.J., 1979, ApJ, 232, 761 CrossRef
Mac Low, M.-M., & Klessen, R.S., 2004, Rev. Mod. Phys., 76, 125 CrossRef
Mookerjea, B., Kramer, C., Nielbock, M., & Nyman, L.-Å., 2004, A&A, 426, 119
Price, S.D., Egan, M.P., Carey, S.J., Mizuno, D.R., & Kuchar, T.A., 2001, AJ, 121, 2819 CrossRef
Rizzo, J.R., Fuente, A., & García-Burillo, S., 2005, ApJ, 634, 1133 CrossRef
Wong, T., Ladd, E.F., Brisbin, D., et al., 2008, MNRAS, in press