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Molecular and ionized gas kinematics in the GC Radio Arc

Published online by Cambridge University Press:  09 February 2017

N. Butterfield ,
C.C. Lang ,
E. A. C. Mills ,
D. Ludovici ,
J. Ott Open the ORCID record for J. Ott [Opens in a new window]  and
M. R. Morris
N. Butterfield
Affiliation:
Dept. of Physics & Astronomy, University of Iowa, USA (email: [email protected])
C.C. Lang
Affiliation:
Dept. of Physics & Astronomy, University of Iowa, USA (email: [email protected])
E. A. C. Mills
Affiliation:
Dept. of Physics & Astronomy, San Jose State University, USA
D. Ludovici
Affiliation:
Dept. of Physics & Astronomy, University of Iowa, USA (email: [email protected])
J. Ott
Affiliation:
National Radio Astronomy Observatory, USA
M. R. Morris
Affiliation:
Dept. of Physics & Astronomy, University of California, Los Angeles, CA, USA
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Abstract

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We present NH3 and H64α+H63α VLA observations of the Radio Arc region, including the M0.20 – 0.033 and G0.10 – 0.08 molecular clouds. These observations suggest the two velocity components of M0.20 – 0.033 are physically connected in the south. Additional ATCA observations suggest this connection is due to an expanding shell in the molecular gas, with the centroid located near the Quintuplet cluster. The G0.10 – 0.08 molecular cloud has little radio continuum, strong molecular emission, and abundant CH3OH masers, similar to a nearby molecular cloud with no star formation: M0.25+0.01. These features detected in G0.10 – 0.08 suggest dense molecular gas with no signs of current star formation.

Keywords

Galaxy: centerISM: cloudsISM: moleculesmasers
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S322: The Multi-Messenger Astrophysics of the Galactic Centre , July 2016 , pp. 133 - 136
Copyright
Copyright © International Astronomical Union 2017 

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