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Detailed distributions of the CO J = (2 − 1)/J = (1 − 0) intensity ratios toward a large area of the central molecular zone

Published online by Cambridge University Press:  22 May 2014

Kazufumi Torii ,
Rei Enokiya ,
Yasuo Fukui ,
Hiroaki Yamamoto ,
Akiko Kawamura ,
Norikazu Mizuno ,
Toshikazu Onishi  and
Hideo Ogawa
Kazufumi Torii
Affiliation:
Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8601, Japan; email: [email protected]
Rei Enokiya
Affiliation:
Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8601, Japan; email: [email protected]
Yasuo Fukui
Affiliation:
Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8601, Japan; email: [email protected]
Hiroaki Yamamoto
Affiliation:
Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8601, Japan; email: [email protected]
Akiko Kawamura
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan
Norikazu Mizuno
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan
Toshikazu Onishi
Affiliation:
Department of Astrophysics, Graduate School of Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, Japan
Hideo Ogawa
Affiliation:
Department of Astrophysics, Graduate School of Science, Osaka Prefecture University, 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, Japan
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Abstract

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We present the first results of the new CO J = (2 − 1) observations toward the central molecular zone (CMZ) using the NANTEN2 telescope at an angular resolution of 100″. Large area coverage of 4° × 2° in l and b and a high angular resolution of 100″ enable us to investigate detailed structures of the molecular gas in the CMZ including peculiar molecular filaments perpendicularly to the Galactic plane to b > |0.5°|. The major components of the CMZ, e.g., Sgr A, Sgr B and Sgr C cloud complexes, show high CO J = (2 − 1)/J = (1 − 0) ratios around 0.9, indicating highly excited conditions of the molecular gas, while the local foreground components show less than 0.4. The molecular filaments show the typical ratios of 0.6–0.7 indicate that they are indeed located in the Galactic center.

Keywords

ISM: clouds — Radio lines: ISM — Galaxy: Galactic center
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S303: The Galactic Center: Feeding and Feedback in a Normal Galactic Nucleus , October 2013 , pp. 106 - 108
Copyright
Copyright © International Astronomical Union 2014 

References

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