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The Environmental Effect of the CMF in the Galactic Center 50 km s−1 Molecular Cloud

Published online by Cambridge University Press:  21 March 2013

Masato Tsuboi  and
Atsushi Miyazaki
Masato Tsuboi
Affiliation:
Institute of Space and Astronautical Science, 3-1-1 Yoshinodai, Sagamihara, 252-5210, Japan email: tsuboi@vsop.isas.jaxa.jp
Atsushi Miyazaki
Affiliation:
Korean VLBI Network, Korea Astronomy and Space Science Institute, P.0. Box 89, Yonsei University, 262 Seongsan-ro, Seodaemun-gu, Seoul 120-749, Korea email: amiya@kasi.re.kr
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Abstract

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We present the statistical properties of molecular clumps in the Galactic center 50 km s−1 molecular cloud based on observations of the CS J = 1 − 0 emission line with the Nobeyama Millimeter Array. The CMF and size spectrum for the whole cloud can be described by power laws of dN/dM ∝ M−2.6 ± 0.1 and dN/dR ∝ R−5.9±0.3, respectively. The CMF observed in the interacting part with the Sgr A East steepens to dN/dM ∝ M−4.0±0.2. On the other hand, the interaction presumably truncates the size spectrum on the larger side of R ∼ 0.4 pc.

Keywords

ISM: clouds — supernova remnants — stars: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S292: Molecular Gas, Dust, and Star Formation in Galaxies , August 2012 , pp. 114
Copyright
Copyright © International Astronomical Union 2013

References

Tsuboi, M., Miyazaki, A., & Okumura, S. K. 2009, PASJ, 61, 29Google Scholar
Bally, J.et al. 2010, ApJ, 721, 137CrossRefGoogle Scholar