Magnetic field structure in Serpens South

DOI PDF 11 Citations 39 References
  • Takayoshi Kusune
    National Astronomical Observatory of Japan, 2-21-1 Osawa , Mitaka, Tokyo 181-8588, Japan
  • Fumitaka Nakamura
    National Astronomical Observatory of Japan, 2-21-1 Osawa , Mitaka, Tokyo 181-8588, Japan
  • Koji Sugitani
    Graduate School of Natural Sciences, Nagoya City University , Mizuho-ku, Nagoya, Aichi 467-8501, Japan
  • Shuji Sato
    Department of Astrophysics, Nagoya University , Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8602, Japan
  • Motohide Tamura
    National Astronomical Observatory of Japan, 2-21-1 Osawa , Mitaka, Tokyo 181-8588, Japan
  • Jungmi Kwon
    Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency , 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210, Japan
  • Kazuhito Dobashi
    Department of Astronomy and Earth Science, Tokyo Gakugei University , 4-1-1 Nukuikita-machi, Koganei, Tokyo 184-8501, Japan
  • Tomomi Shimoikura
    Department of Astronomy and Earth Science, Tokyo Gakugei University , 4-1-1 Nukuikita-machi, Koganei, Tokyo 184-8501, Japan
  • Benjamin Wu
    National Astronomical Observatory of Japan, 2-21-1 Osawa , Mitaka, Tokyo 181-8588, Japan

Description

<jats:title>Abstract</jats:title> <jats:p>We made near-infrared polarimetric observations toward Serpens South. This region contains three dense filaments that are roughly parallel to one another. Using the histogram of relative orientations, the three filaments are found to be roughly perpendicular to the global magnetic field. The morphology of the plane-of-sky (POS) magnetic field and molecular gas suggests that the magnetic field plays an important role in the filament formation and evolution. Applying the Davis–Chandrasekhar–Fermi method, the POS magnetic field strengths are estimated to be 10–80$\, \mu$G. The evaluated mass-to-flux ratios indicate that the center filament is magnetically supercritical, while the others are approximately magnetically critical. We speculate that the filaments are formed by fragmentation of a sheet-like cloud that was created through the gravitational contraction of a magnetized, turbulent cloud.</jats:p>

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