A Tale of three: Magnetic fields along the Orion integral-shaped filament as revealed by the JCMT BISTRO survey

Wu, Jintai, Qiu, Keping, Poidevin, Frédérick, Bastien, Pierre, Liu, Junhao, Ching, Tao-Chung, Bourke, Tyler L., Ward-Thompson, Derek, Pattle, Kate, Johnstone, Doug, Koch, Patrick M., Arzoumanian, Doris, Lee, Chang Won, Fanciullo, Lapo, Onaka, Takashi, Hwang, Jihye, Gouellec, Valentin J. M. Le, Soam, Archana, Tamura, Motohide, Tahani, Mehrnoosh, Eswaraiah, Chakali, Li, Hua-Bai, Berry, David, Furuya, Ray S., Coudé, Simon, Kwon, Woojin, Lin, Sheng-Jun, Wang, Jia-Wei, Hasegawa, Tetsuo, Lai, Shih-Ping, Byun, Do-Young, Chen, Zhiwei, Chen, Huei-Ru Vivien, Chen, Wen Ping, Chen, Mike, Cho, Jungyeon, Choi, Youngwoo, Choi, Yunhee, Choi, Minho, Chrysostomou, Antonio, Chung, Eun Jung, Dai, Sophia, Francesco, James Di, Diep, Pham Ngoc, Doi, Yasuo, Duan, Hao-Yuan, Duan, Yan, Eden, David, Fiege, Jason, Fissel, Laura M., Franzmann, Erica, Friberg, Per, Friesen, Rachel, Fuller, Gary, Gledhill, Tim, Graves, Sarah, Greaves, Jane, Griffin, Matt ORCID: https://orcid.org/0000-0002-0033-177X, Gu, Qilao, Han, Ilseung, Hayashi, Saeko, Hoang, Thiem, Houde, Martin, Inoue, Tsuyoshi, Inutsuka, Shu-ichiro, Iwasaki, Kazunari, Jeong, Il-Gyo, Könyves, Vera, Kang, Ji-hyun, Kang, Miju, Karoly, Janik, Kataoka, Akimasa, Kawabata, Koji, Kim, Shinyoung, Kim, Mi-Ryang, Kim, Kyoung Hee, Kim, Kee-Tae, Kim, Jongsoo, Kim, Hyosung, Kim, Gwanjeong, Kirchschlager, Florian, Kirk, Jason, Kobayashi, Masato I.N., Kusune, Takayoshi, Kwon, Jungmi, Lacaille, Kevin, Law, Chi-Yan, Lee, Hyeseung, Lee, Chin-Fei, Lee, Sang-Sung, Lee, Jeong-Eun, Li, Dalei, Li, Di, Li, Guangxing, Liu, Sheng-Yuan, Liu, Tie, Liu, Hong-Li, Lu, Xing, Lyo, A-Ran, Mairs, Steve, Matsumura, Masafumi, Matthews, Brenda, Moriarty-Schieven, Gerald, Nagata, Tetsuya, Nakamura, Fumitaka, Nakanishi, Hiroyuki, Ngoc, Nguyen Bich, Ohashi, Nagayoshi, Park, Geumsook, Parsons, Harriet, Peretto, Nicolas ORCID: https://orcid.org/0000-0002-6893-602X, Priestley, Felix, Pyo, Tae-Soo, Qian, Lei, Rao, Ramprasad, Rawlings, Jonathan, Rawlings, Mark, Retter, Brendan, Richer, John, Rigby, Andrew, Sadavoy, Sarah, Saito, Hiro, Savini, Giorgio, Seta, Masumichi, Sharma, Ekta, Shimajiri, Yoshito, Shinnaga, Hiroko, Tang, Ya-Wen, Tang, Xindi, Thuong, Hoang Duc, Tomisaka, Kohji, Tram, Le Ngoc, Tsukamoto, Yusuke, Viti, Serena, Wang, Hongchi, Whitworth, Anthony ORCID: https://orcid.org/0000-0002-1178-5486, Xie, Jinjin, Yang, Meng-Zhe, Yen, Hsi-Wei, Yoo, Hyunju, Yuan, Jinghua, Yun, Hyeong-Sik, Zenko, Tetsuya, Zhang, Guoyin, Zhang, Chuan-Peng, Zhang, Yapeng, Zhou, Jianjun, Zhu, Lei, Looze, Ilse de, André, Philippe, Dowell, C. Darren, Eyres, Stewart, Falle, Sam, Robitaille, Jean-François and van Loo, Sven 2024. A Tale of three: Magnetic fields along the Orion integral-shaped filament as revealed by the JCMT BISTRO survey. The Astrophysical Journal Letters 977 (2) , L31. 10.3847/2041-8213/ad93d2

Preview

PDF - Published Version Available under License Creative Commons Attribution. Download (13MB) | Preview

Abstract

As part of the B-fields In Star-forming Region Observations survey, we present James Clerk Maxwell Telescope (JCMT) 850 μm 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.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Schools > Physics and Astronomy
ISSN:	2040-8205
Funders:	National Natural Science Foundation of China
Date of First Compliant Deposit:	25 February 2025
Date of Acceptance:	17 November 2024
Last Modified:	25 Feb 2025 10:04
URI:	https://orca.cardiff.ac.uk/id/eprint/174912

Actions (repository staff only)

Edit Item