Near-infrared imaging polarimetry toward M 17 SWex

DOI DOI PDF 被引用文献9件 参考文献77件
  • Koji Sugitani
    Graduate School of Natural Sciences, Nagoya City University , Mizuho-ku, Nagoya, Aichi 467-8501, Japan
  • Fumitaka Nakamura
    National Astronomical Observatory , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
  • Tomomi Shimoikura
    Department of Astronomy and Earth Science, Tokyo Gakugei University , Koganei, Tokyo 184-8501, Japan
  • Kazuhito Dobashi
    Department of Astronomy and Earth Science, Tokyo Gakugei University , Koganei, Tokyo 184-8501, Japan
  • Quang Nguyen-Luong
    Graduate School of Natural Sciences, Nagoya City University , Mizuho-ku, Nagoya, Aichi 467-8501, Japan
  • Takayoshi Kusune
    National Astronomical Observatory , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
  • Takahiro Nagayama
    Kagoshima University , 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065, Japan
  • Makoto Watanabe
    Department of Applied Physics, Okayama University of Science , 1-1 Ridai-cho, Kita-ku, Okayama, Okayama 700-0005, Japan
  • Shogo Nishiyama
    Miyagi University of Education, 149 Aramaki-aza-Aoba , Aobaku, Sendai, Miyagi 980-0845, Japan
  • Motohide Tamura
    National Astronomical Observatory , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

この論文をさがす

説明

<jats:title>Abstract</jats:title><jats:p>We conducted near-infrared ($\mathit {JHK}_{\rm s}$) imaging polarimetry toward the infrared dark cloud (IRDC) M 17 SWex, including almost all of the IRDC filaments as well as its outskirts, with the polarimeter SIRPOL on the IRSF 1.4 m telescope. We revealed the magnetic fields of M 17 SWex with our polarization-detected sources that were selected by some criteria based on their near-IR colors and the column densities toward them, which were derived from the Herschel data. The selected sources indicate not only that the ordered magnetic field is perpendicular to the cloud elongation as a whole, but also that at both ends of the elongated cloud the magnetic field appears to be bent toward its central part, i.e., a large-scale hourglass-shaped magnetic field perpendicular to the cloud elongation. In addition to this general trend, the elongations of the filamentary subregions within the dense parts of the cloud appear to be mostly perpendicular to their local magnetic fields, while the magnetic fields of the outskirts appear to follow the thin filaments that protrude from the dense parts. The magnetic strengths were estimated to be ∼70–$300\, \mu$G in the subregions, of which the lengths and average number densities are ∼3–9 pc and ∼2–7 × 103 cm−3, respectively, by the Davis–Chandrasekhar–Fermi method with the angular dispersion of our polarization data and the velocity dispersion derived from the C18O (J = 1–0) data obtained by the Nobeyama 45 m telescope. These field configurations and our magnetic stability analysis of the subregions imply that the magnetic field has controlled the formation/evolution of the M 17 SWex cloud.</jats:p>

収録刊行物

被引用文献 (9)*注記

もっと見る

参考文献 (77)*注記

もっと見る

関連プロジェクト

もっと見る

キーワード

詳細情報 詳細情報について

問題の指摘

ページトップへ