Magnetic Field of a Ring-like Molecular Cloud

Alina D. Umirbayeva A. Doi Y. Jo S. Hu Y. Lazarian A. Karoly J. Liu T. Kawabata K.S. Mukhash A. Zhumagayir D. Hori T. Maruta T. Imazawa R. Nakaoka T. Sasada M.
1 September 2025 American Astronomical Society

Astronomical Journal
2025 #170 Issue 3

We present a detailed study of the magnetic field structure in the G111 molecular cloud, a ring-like filamentary cloud within the NGC 7538 region. Our analysis combines multiwavelength polarization data and molecular-line observations to investigate the magnetic field’s role in the cloud’s formation and evolution. We utilized interstellar dust polarization from the Planck telescope to trace large-scale field orientations, starlight extinction polarization from the Kanata telescope to probe the cloud’s magnetic field after foreground subtraction, and velocity gradients derived from CO isotopologues observed with the IRAM 30 m telescope to examine dense regions. Our results reveal a coherent yet spatially varying magnetic field within G111. The alignment between Planck-derived orientations and starlight extinction polarization highlights significant foreground dust contamination, which we correct through careful subtraction. The global alignment of the magnetic field with density structures suggests that the field is dynamically important in shaping the cloud. Variations in CO-derived orientations further suggest that local dynamical effects, such as gravitational interactions and turbulence, influence the cloud’s structure. The curved magnetic field along the dense ridges, coinciding with mid-infrared emission in WISE data, indicates shock compression, likely driven by stellar feedback or supernova remnants. Our findings support a scenario where G111’s morphology results from turbulent shock-driven compression, rather than simple gravitational contraction. The interplay between magnetic fields and external forces is crucial in shaping molecular clouds and regulating star formation. Future high-resolution observations will be essential to further constrain the magnetic field’s role in cloud evolution.

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Kabanbay batyr ave, 53, Astana, 010000, Kazakhstan
Laboratory of Physics of Stars and Nebulae, Fesenkov Astrophysical Institute, Observatory 23, Almaty, 050020, Kazakhstan
Department of Earth Science and Astronomy, Graduate School of Arts and Sciences, The University of Tokyo, 3-8-1 Komaba, Meguro, Tokyo, 153-8902, Japan
Institute for Advanced Study, 1 Einstein Drive, Princeton, 08540, NJ, United States
Department of Astronomy, University of Wisconsin-Madison, Madison, 53706, WI, United States
Department of Physics and Astronomy, University College London, London, WC1E 6BT, United Kingdom
Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai, 200030, China
Hiroshima Astrophysical Science Center, Hiroshima University, 1-3-1 Kagamiyama Higashi-Hiroshima, Hiroshima, 739-8526, Japan
Physics Program, Graduate School of Advanced Science and Engineering, Hiroshima University, 1-3-1 Kagamiyama Higashi-Hiroshima, Hiroshima, 739-8526, Japan
Math Department, School of Sciences and Humanities, Nazarbayev University, Kabanbay batyr ave, 53, Astana, 010000, Kazakhstan
Institute of Innovative Research, Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo, 152-8551, Japan

Kabanbay batyr ave
Laboratory of Physics of Stars and Nebulae
Department of Earth Science and Astronomy
Institute for Advanced Study
Department of Astronomy
Department of Physics and Astronomy
Key Laboratory for Research in Galaxies and Cosmology
Hiroshima Astrophysical Science Center
Physics Program
Math Department
Institute of Innovative Research

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