JCMT BISTRO Survey: Magnetic Fields within the Hub-filament Structure in IC 5146

Wang, Jia-Wei, Lai, Shih-Ping, Eswaraiah, Chakali, Pattle, Kate, Francesco, James Di, Johnstone, Doug, Koch, Patrick M., Liu, Tie, Tamura, Motohide, Furuya, Ray S., Onaka, Takashi, Ward-Thompson, Derek, Soam, Archana, Kim, Kee-Tae, Lee, Chang Won, Lee, Chin-Fei, Mairs, Steve, Arzoumanian, Doris, Kim, Gwanjeong, Hoang, Thiem, Hwang, Jihye, Liu, Sheng-Yuan, Berry, David, Bastien, Pierre, Hasegawa, Tetsuo, Kwon, Woojin, Qiu, Keping, André, Philippe, Aso, Yusuke, Byun, Do-Young, Chen, Huei-Ru, Chen, Michael C., Chen, Wen Ping, Ching, Tao-Chung, Cho, Jungyeon, Choi, Minho, Chrysostomou, Antonio, Chung, Eun Jung, Coudé, Simon, Doi, Yasuo, Dowell, C. Darren, Drabek-Maunder, Emily ORCID: https://orcid.org/0000-0002-3476-2260, Duan, Hao-Yuan, Eyres, Stewart P. S., Falle, Sam, Fanciullo, Lapo, Fiege, Jason, Franzmann, Erica, Friberg, Per, Friesen, Rachel K., Fuller, Gary, Gledhill, Tim, Graves, Sarah F., Greaves, Jane S. ORCID: https://orcid.org/0000-0002-3133-413X, Griffin, Matt J. ORCID: https://orcid.org/0000-0002-0033-177X, Gu, Qilao, Han, Ilseung, Hatchell, Jennifer, Hayashi, Saeko S., Holland, Wayne, Houde, Martin, Inoue, Tsuyoshi, Inutsuka, Shu-ichiro, Iwasaki, Kazunari, Jeong, Il-Gyo, Kanamori, Yoshihiro, Kang, Ji-hyun, Kang, Miju, Kang, Sung-ju, Kataoka, Akimasa, Kawabata, Koji S., Kemper, Francisca, Kim, Jongsoo, Kim, Kyoung Hee, Kim, Mi-Ryang, Kim, Shinyoung, Kirk, Jason M., Kobayashi, Masato I. N., Konyves, Vera, Kwon, Jungmi, Lacaille, Kevin M., Lee, Hyeseung, Lee, Jeong-Eun, Lee, Sang-Sung, Lee, Yong-Hee, Li, Dalei, Li, Di, Li, Hua-bai, Liu, Hong-Li, Liu, Junhao, Lyo, A-Ran, Matsumura, Masafumi, Matthews, Brenda C., Moriarty-Schieven, Gerald H., Nagata, Tetsuya, Nakamura, Fumitaka, Nakanishi, Hiroyuki, Ohashi, Nagayoshi, Park, Geumsook, Parsons, Harriet, Pascale, Enzo ORCID: https://orcid.org/0000-0002-3242-8154, Peretto, Nicolas ORCID: https://orcid.org/0000-0002-6893-602X, Pon, Andy, Pyo, Tae-Soo, Qian, Lei, Rao, Ramprasad, Rawlings, Mark G., Retter, Brendan, Richer, John, Rigby, Andrew, Robitaille, Jean-François, Sadavoy, Sarah, Saito, Hiro, Savini, Giorgio, Scaife, Anna M. M., Seta, Masumichi, Shinnaga, Hiroko, Tang, Ya-Wen, Tomisaka, Kohji, Tsukamoto, Yusuke, Loo, Sven van, Wang, Hongchi, Whitworth, Anthony P. ORCID: https://orcid.org/0000-0002-1178-5486, Yen, Hsi-Wei, Yoo, Hyunju, Yuan, Jinghua, Yun, Hyeong-Sik, Zenko, Tetsuya, Zhang, Chuan-Peng, Zhang, Guoyin, Zhang, Ya-Peng, Zhou, Jianjun and Zhu, Lei 2019. JCMT BISTRO Survey: Magnetic Fields within the Hub-filament Structure in IC 5146. Astrophysical Journal 876 (1) , 42. 10.3847/1538-4357/ab13a2

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Abstract

We present the 850 μm polarization observations toward the IC 5146 filamentary cloud taken using the Submillimetre Common-User Bolometer Array 2 (SCUBA-2) and its associated polarimeter (POL-2), mounted on the James Clerk Maxwell Telescope, as part of the B-fields In STar forming Regions Observations. This work is aimed at revealing the magnetic field morphology within a core-scale (lesssim1.0 pc) hub-filament structure (HFS) located at the end of a parsec-scale filament. To investigate whether the observed polarization traces the magnetic field in the HFS, we analyze the dependence between the observed polarization fraction and total intensity using a Bayesian approach with the polarization fraction described by the Rice likelihood function, which can correctly describe the probability density function of the observed polarization fraction for low signal-to-noise ratio data. We find a power-law dependence between the polarization fraction and total intensity with an index of 0.56 in A V ~ 20–300 mag regions, suggesting that the dust grains in these dense regions can still be aligned with magnetic fields in the IC 5146 regions. Our polarization maps reveal a curved magnetic field, possibly dragged by the contraction along the parsec-scale filament. We further obtain a magnetic field strength of 0.5 ± 0.2 mG toward the central hub using the Davis–Chandrasekhar–Fermi method, corresponding to a mass-to-flux criticality of ~1.3 ± 0.4 and an Alfvénic Mach number of <0.6. These results suggest that gravity and magnetic field are currently of comparable importance in the HFS and that turbulence is less important.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Schools > Physics and Astronomy
Publisher:	American Astronomical Society
ISSN:	0004-637X
Date of First Compliant Deposit:	14 May 2019
Date of Acceptance:	25 March 2019
Last Modified:	05 Dec 2023 02:49
URI:	https://orca.cardiff.ac.uk/id/eprint/122434

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