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Propagation of Highly Efficient Star Formation in the North American Nebula (NGC 7000)

Published online by Cambridge University Press:  21 March 2013

Hideyuki Toujima ,
Toshihiro Handa ,
Toshihiro Omodaka ,
Takumi Nagayama ,
Hideyuki Kobayashi  and
Yasuhiro Koyama
Hideyuki Toujima
Affiliation:
Depart. Astron. & Phys., Kagoshima Univ., Korimoto 1-21-35, Kagoshima 890-0065, Japan email: handa@sci.kagoshima-u.ac.jp
Toshihiro Handa
Affiliation:
Depart. Astron. & Phys., Kagoshima Univ., Korimoto 1-21-35, Kagoshima 890-0065, Japan email: handa@sci.kagoshima-u.ac.jp
Toshihiro Omodaka
Affiliation:
Depart. Astron. & Phys., Kagoshima Univ., Korimoto 1-21-35, Kagoshima 890-0065, Japan email: handa@sci.kagoshima-u.ac.jp
Takumi Nagayama
Affiliation:
National Astronomical Observatory of Japan
Hideyuki Kobayashi
Affiliation:
National Astronomical Observatory of Japan
Yasuhiro Koyama
Affiliation:
National Institute of Information and Communications Technology
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Abstract

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We mapped the molecular cloud associated with the North American Nebula in the NH3 lines and the H2O maser using the Kashima 34-m telescope. The line ratio shows the molecular gas is cold. For the clumps and subclumps in the cloud we also estimate the star forming efficiency (SFE). The east end of the cloud shows the highest SEF, 0.62, and the other end is the lowest, 0.06. The 3 dimensional structure derived using the published Hα map suggests the east end is in the HII region and it should be a reason why the SFE is high there.

Keywords

ISM: individual (North American Nebula) — ISM: molecules — radio lines: ISM
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. 59
Copyright
Copyright © International Astronomical Union 2013

References

Fountain, W. F., Gray, G. A., & O'Dell, C. R. 1983, ApJ, 269, 164Google Scholar
Toujima, H., et al. 2011, PASJ, 63, 1259CrossRefGoogle Scholar