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Large–scale and high–sensitivity multi–line CO surveys toward the Galactic center

Published online by Cambridge University Press:  22 May 2014

R. Enokiya ,
K. Torii ,
M. Schultheis ,
Y. Asahina ,
R. Matsumoto ,
H. Yamamoto ,
K. Tachihara ,
T. Okuda ,
M. R. Morris  and
Y. Fukui
R. Enokiya
Affiliation:
Department of Physics and Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi, 464-8601, Japan email: [email protected]
K. Torii
Affiliation:
Department of Physics and Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi, 464-8601, Japan email: [email protected]
M. Schultheis
Affiliation:
Observatoire de la Cote d'Azur Laboratoire Lagrange, CNRS UMR 7293, B. P. 4229 06304 Nice Cedex 04, France
Y. Asahina
Affiliation:
Faculty of Science, Chiba University, Inage-ku, Chiba 263-8522
R. Matsumoto
Affiliation:
Faculty of Science, Chiba University, Inage-ku, Chiba 263-8522
H. Yamamoto
Affiliation:
Department of Physics and Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi, 464-8601, Japan email: [email protected]
K. Tachihara
Affiliation:
Department of Physics and Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi, 464-8601, Japan email: [email protected]
T. Okuda
Affiliation:
National Astronomical Observatory of Japan, Mitaka, Tokyo, 181-8588, Japan
M. R. Morris
Affiliation:
Department of Physics and Astronomy, University of California, Los Angeles, California 90095-1547, USA
Y. Fukui
Affiliation:
Department of Physics and Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi, 464-8601, Japan email: [email protected]
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Abstract

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We carried out large–scale (4 × 2 degree) CO multi–line observations toward the central molecular zone (CMZ) in the Galactic center (GC) with the NANTEN2 4m telescope and mapped several diffuse molecular features located at relatively high Galactic latitudes above 0°.6. These high–latitude features are composed of diffuse molecular halo gas and molecular filaments according to their morphological aspects. Their high velocities and high intensity ratios between 12CO J = (2−1) and J = (1−0) clearly indicate their location in the GC, and their total mass amount to ∼10% of that of the CMZ. We discuss that magnetic field is a possible mechanism of these high–latitude molecular features lifting up toward high galactic latitude.

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. 194 - 198
Copyright
Copyright © International Astronomical Union 2014 

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