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Nobeyama 45m CO Galactic Plane Survey: Filament properties and star formation in M17

Published online by Cambridge University Press:  12 September 2016

Atsushi Nishimura
Affiliation:
Nobeyama Radio Observatory, National Astronomical Observatory of Japan, Minamimaki, Minamisaku, Nagano, Japan
Tomofumi Umemoto
Affiliation:
Nobeyama Radio Observatory, National Astronomical Observatory of Japan, Minamimaki, Minamisaku, Nagano, Japan
Tetsuhiro Minamidani
Affiliation:
Nobeyama Radio Observatory, National Astronomical Observatory of Japan, Minamimaki, Minamisaku, Nagano, Japan
Nario Kuno
Affiliation:
Department of Physics, Graduate School of Pure and Applied Sciences, University of Tsukuba, Tsukuba, Ibaraki, Japan Center for Integrated Research in Fundamental Science and Engineering (CiRfSE), University of Tsukuba, Tsukuba, Ibaraki, Japan
Tomoka Tosaki
Affiliation:
Department of Geoscience, Joetsu University of Education, Joetsu, Niigata, Japan
Shinji Fujita
Affiliation:
Department of Physics, Graduate School of Pure and Applied Sciences, University of Tsukuba, Tsukuba, Ibaraki, Japan
Mitsuhiro Matsuo
Affiliation:
Graduate School of Science and Engineering, Kagoshima University, Kagoshima, Kagoshima, Japan
Yuya Tsuda
Affiliation:
Graduate School of Science and Engineering, Meisei University, Hino, Tokyo, Japan
Satoshi Ohashi
Affiliation:
Department of Astronomy, The University of Tokyo, Bunkyo-ku, Tokyo, Japan email: atsushi.nishimura@nao.ac.jp
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Abstract

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We present the 12CO J=1–0, 13CO J=1–0, and C18O J=1–0 maps of the M17 giant molecular clouds (GMCs) obtained as a part of the Nobeyama 45m CO Galactic Plane Survey. The observations cover the entire area of M17 SW and M17 N clouds at an angular resolution of ~ 15″ which corresponds to ~ 0.15 pc. We found that the N cloud consists of a couple of twisted filaments, they are extended in parallel toward the Hii region. The typicall width of the filaments is ~0.5 pc in 13CO intensity map. Most of young stellar objects (YSOs) are located on the filaments which have a bright rim structure in 8μm at the filament edge facing the Hii region. Furthermore, the time scale of the YSOs formation on the bright rim is comparable with that of NGC 6618 cluster which provides UV photons for the region. This fact indicates that the cluster triggered to form YSOs in N cloud. We also investigated the geometry of the Hii region and GMCs by comparing spatial distribution of 12CO velocity channel map and infrared dark cloud, and then found that NGC 6618 is possibly formed by the cloud cloud colision.

Type
Poster Papers
Copyright
Copyright © International Astronomical Union 2016 

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