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A Large-Scale CO Imaging of the Galactic Center

  • T. Oka (a1), T. Hasegawa (a2), F. Sato (a3), H. Yamasaki (a3), M. Tsuboi (a4) and A. Miyazaki (a4)...

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Molecular gas in the Galactic center region is spatially and kinematically complex, and its physical conditions are distinctively different from those of molecular gas in the Galactic disk (e.g., Morris 1996). Relative paucity of current star formation activity, despite the abundance of dense molecular gas in this region, is one of the problem at issue.

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Copyright

References

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Hasegawa, T. et al. 1996, Nature, submitted.
Heckman, T. M., Lehnert, M. D., and Armus, L. 1993, in “The Environment and Evolution of Galaxies,” eds. Shull, J. M. and Thronson, H. A. Jr. (Dordrecht: Kluwer), 455.
Lindqvist, M., Winnberg, A., Habing, H.J., and Matthews, H.E. 1991, Astron. Astrophys. Suppl., 92, 43.
Morris, M. 1996, in IAU Symposium 170, “CO: Twenty-five Years of Millimeter-wave Spectroscopy,” in press.
Oka, T., Hasegawa, T., Sato, F., Tsuboi, M., and Handa, T. 1996, in IAU Symposium 170, “CO: Twenty-five Years of Millimeter-wave Spectroscopy,” in press.

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