The Astrophysical Journal Letters (Jan 2024)

A Tale of Three: Magnetic Fields along the Orion Integral-shaped Filament as Revealed by the JCMT BISTRO Survey

  • Jintai Wu,
  • Keping Qiu,
  • Frédérick Poidevin,
  • Pierre Bastien,
  • Junhao Liu,
  • Tao-Chung Ching,
  • Tyler L. Bourke,
  • Derek Ward-Thompson,
  • Kate Pattle,
  • Doug Johnstone,
  • Patrick M. Koch,
  • Doris Arzoumanian,
  • Chang Won Lee,
  • Lapo Fanciullo,
  • Takashi Onaka,
  • Jihye Hwang,
  • Valentin J. M. Le Gouellec,
  • Archana Soam,
  • Motohide Tamura,
  • Mehrnoosh Tahani,
  • Chakali Eswaraiah,
  • Hua-Bai Li,
  • David Berry,
  • Ray S. Furuya,
  • Simon Coudé,
  • Woojin Kwon,
  • Sheng-Jun Lin,
  • Jia-Wei Wang,
  • Tetsuo Hasegawa,
  • Shih-Ping Lai,
  • Do-Young Byun,
  • Zhiwei Chen,
  • Huei-Ru Vivien Chen,
  • Wen Ping Chen,
  • Mike Chen,
  • Jungyeon Cho,
  • Youngwoo Choi,
  • Yunhee Choi,
  • Minho Choi,
  • Antonio Chrysostomou,
  • Eun Jung Chung,
  • Sophia Dai,
  • James Di Francesco,
  • Pham Ngoc Diep,
  • Yasuo Doi,
  • Hao-Yuan Duan,
  • Yan Duan,
  • David Eden,
  • Jason Fiege,
  • Laura M. Fissel,
  • Erica Franzmann,
  • Per Friberg,
  • Rachel Friesen,
  • Gary Fuller,
  • Tim Gledhill,
  • Sarah Graves,
  • Jane Greaves,
  • Matt Griffin,
  • Qilao Gu,
  • Ilseung Han,
  • Saeko Hayashi,
  • Thiem Hoang,
  • Martin Houde,
  • Tsuyoshi Inoue,
  • Shu-ichiro Inutsuka,
  • Kazunari Iwasaki,
  • Il-Gyo Jeong,
  • Vera Könyves,
  • Ji-hyun Kang,
  • Miju Kang,
  • Janik Karoly,
  • Akimasa Kataoka,
  • Koji Kawabata,
  • Shinyoung Kim,
  • Mi-Ryang Kim,
  • Kyoung Hee Kim,
  • Kee-Tae Kim,
  • Jongsoo Kim,
  • Hyosung Kim,
  • Gwanjeong Kim,
  • Florian Kirchschlager,
  • Jason Kirk,
  • Masato I.N. Kobayashi,
  • Takayoshi Kusune,
  • Jungmi Kwon,
  • Kevin Lacaille,
  • Chi-Yan Law,
  • Hyeseung Lee,
  • Chin-Fei Lee,
  • Sang-Sung Lee,
  • Jeong-Eun Lee,
  • Dalei Li,
  • Di Li,
  • Guangxing Li,
  • Sheng-Yuan Liu,
  • Tie Liu,
  • Hong-Li Liu,
  • Xing Lu,
  • A-Ran Lyo,
  • Steve Mairs,
  • Masafumi Matsumura,
  • Brenda Matthews,
  • Gerald Moriarty-Schieven,
  • Tetsuya Nagata,
  • Fumitaka Nakamura,
  • Hiroyuki Nakanishi,
  • Nguyen Bich Ngoc,
  • Nagayoshi Ohashi,
  • Geumsook Park,
  • Harriet Parsons,
  • Nicolas Peretto,
  • Felix Priestley,
  • Tae-Soo Pyo,
  • Lei Qian,
  • Ramprasad Rao,
  • Jonathan Rawlings,
  • Mark Rawlings,
  • Brendan Retter,
  • John Richer,
  • Andrew Rigby,
  • Sarah Sadavoy,
  • Hiro Saito,
  • Giorgio Savini,
  • Masumichi Seta,
  • Ekta Sharma,
  • Yoshito Shimajiri,
  • Hiroko Shinnaga,
  • Ya-Wen Tang,
  • Xindi Tang,
  • Hoang Duc Thuong,
  • Kohji Tomisaka,
  • Le Ngoc Tram,
  • Yusuke Tsukamoto,
  • Serena Viti,
  • Hongchi Wang,
  • Anthony Whitworth,
  • Jinjin Xie,
  • Meng-Zhe Yang,
  • Hsi-Wei Yen,
  • Hyunju Yoo,
  • Jinghua Yuan,
  • Hyeong-Sik Yun,
  • Tetsuya Zenko,
  • Guoyin Zhang,
  • Chuan-Peng Zhang,
  • Yapeng Zhang,
  • Jianjun Zhou,
  • Lei Zhu,
  • Ilse de Looze,
  • Philippe André,
  • C. Darren Dowell,
  • Stewart Eyres,
  • Sam Falle,
  • Jean-François Robitaille,
  • Sven van Loo

DOI
https://doi.org/10.3847/2041-8213/ad93d2
Journal volume & issue
Vol. 977, no. 2
p. L31

Abstract

Read online

As part of the B -fields In Star-forming Region Observations survey, we present James Clerk Maxwell Telescope (JCMT) 850 μ m polarimetric observations toward the Orion integral-shaped filament (ISF) that covers three portions known as OMC-1, OMC-2, and OMC-3. The magnetic field threading the ISF seen in the JCMT POL-2 map appears as a tale of three: pinched for OMC-1, twisted for OMC-2, and nearly uniform for OMC-3. A multiscale analysis shows that the magnetic field structure in OMC-3 is very consistent at all the scales, whereas the field structure in OMC-2 shows no correlation across different scales. In OMC-1, the field retains its mean orientation from large to small scales but shows some deviations at small scales. Histograms of relative orientations between the magnetic field and filaments reveal a bimodal distribution for OMC-1, a relatively random distribution for OMC-2, and a distribution with a predominant peak at 90 ^∘ for OMC-3. Furthermore, the magnetic fields in OMC-1 and OMC-3 both appear to be aligned perpendicular to the fibers, which are denser structures within the filament, but the field in OMC-2 is aligned along with the fibers. All these suggest that gravity, turbulence, and magnetic field are each playing a leading role in OMC-1, 2, and 3, respectively. While OMC-2 and 3 have almost the same gas mass, density, and nonthermal velocity dispersion, there are on average younger and fewer young stellar objects in OMC-3, providing evidence that a stronger magnetic field will induce slower and less efficient star formation in molecular clouds.

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