The Astrophysical Journal (Jan 2025)

The JCMT BISTRO-3 Survey: Variation of Magnetic Field Orientations on Parsec and Subparsec Scales in the Massive Star-forming Region G28.34+0.06

  • Jihye Hwang,
  • Kate Pattle,
  • Chang Won Lee,
  • Janik Karoly,
  • Kee-Tae Kim,
  • Jongsoo Kim,
  • Junhao Liu,
  • Keping Qiu,
  • A-Ran Lyo,
  • David Eden,
  • Patrick M. Koch,
  • Doris Arzoumanian,
  • Ekta Sharma,
  • Frédérick Poidevin,
  • Doug Johnstone,
  • Simon Coudé,
  • Mehrnoosh Tahani,
  • Derek Ward-Thompson,
  • Archana Soam,
  • Ji-hyun Kang,
  • Thiem Hoang,
  • Woojin Kwon,
  • Nguyen Bich Ngoc,
  • Eun Jung Chung,
  • Tyler L. Bourke,
  • Takashi Onaka,
  • Florian Kirchschlager,
  • Motohide Tamura,
  • Jungmi Kwon,
  • Xindi Tang,
  • Eswaraiah Chakali,
  • Tie Liu,
  • Pierre Bastien,
  • Ray S. Furuya,
  • Shih-Ping Lai,
  • Sheng-Jun Lin,
  • Jia-Wei Wang,
  • David Berry

DOI
https://doi.org/10.3847/1538-4357/adce80
Journal volume & issue
Vol. 985, no. 2
p. 222

Abstract

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Magnetic fields play a significant role in star-forming processes on core to clump scales. We investigate magnetic field orientations and strengths in the massive star-forming clump P2 within the filamentary infrared dark cloud G28.34+0.06 using dust polarization observations made using SCUBA-2/POL-2 on the James Clerk Maxwell Telescope (JCMT) as part of the B-field In STar-forming Region Observations (or BISTRO) survey. We compare the magnetic field orientations at the clump scale of ∼2 pc from these JCMT observations with those at the core scale of ∼0.2 pc from archival Atacama Large Millimeter/submillimeter Array data, finding that the magnetic field orientations on these two different scales are perpendicular to one another. We estimate the distribution of magnetic field strengths, which range from 50 to 430 μ G over the clump. The region forming the core shows the highest magnetic field strength. We also obtain the distribution of mass-to-flux ratios across the clump. In the region surrounding the core, the mass-to-flux ratio is larger than 1, which indicates that the magnetic field strength is insufficient to support the region against gravitational collapse. Therefore, the change in the magnetic field orientation from clump to core scales may be the result of gravitational collapse, with the field being pulled inward along with the flow of material under gravity.

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