B-fields in Star-Forming Region Observations (BISTRO): Magnetic Fields in the Filamentary Structures of Serpens Main
Creators: name: Kwon, Woojin
name: Pattle, Kate
name: Sadavoy, Sarah
name: Hull, Charles L. H.
name: Johnstone, Doug
name: Ward-Thompson, Derek
name: Di Francesco, James
name: Koch, Patrick M.
name: Furuya, Ray
name: Doi, Yasuo
name: Gouellec, Valentin J. M. Le
name: Hwang, Jihye
name: Lyo, A-Ran
name: Soam, Archana
name: Tang, Xindi
name: Hoang, Thiem
name: Kirchschlager, Florian
name: Eswaraiah, Chakali
name: Fanciullo, Lapo
name: Kim, Kyoung Hee
name: Onaka, Takashi
name: Könyves, Vera
name: Kang, Ji-hyun
name: Lee, Chang Won
name: Tamura, Motohide
name: Bastien, Pierre
name: Hasegawa, Tetsuo
name: Lai, Shih-Ping
name: Qiu, Keping
name: Berry, David
name: Arzoumanian, Doris
name: Bourke, Tyler L.
name: Byun, Do-Young
name: Chen, Wen Ping
name: Chen, Huei-Ru Vivien
name: Chen, Mike
name: Chen, Zhiwei
name: Ching, Tao-Chung
name: Cho, Jungyeon
name: Choi, Yunhee
name: Choi, Minho
name: Chrysostomou, Antonio
name: Chung, Eun Jung
name: Coudé, Simon
name: Dai, Sophia
name: Diep, Pham Ngoc
name: Duan, Yan
name: Duan, Hao-Yuan
name: Eden, David
name: Fiege, Jason
name: Fissel, Laura M.
name: Franzmann, Erica
name: Friberg, Per
name: Friesen, Rachel
name: Fuller, Gary
name: Gledhill, Tim
name: Graves, Sarah
name: Greaves, Jane
name: Griffin, Matt
name: Gu, Qilao
name: Han, Ilseung
name: Hatchell, Jennifer
name: Hayashi, Saeko
name: Houde, Martin
name: Inoue, Tsuyoshi
name: Inutsuka, Shu-ichiro
name: Iwasaki, Kazunari
name: Jeong, Il-Gyo
name: Kang, Miju
name: Karoly, Janik
name: Kataoka, Akimasa
name: Kawabata, Koji
name: Kemper, Francisca
name: Kim, Kee-Tae
name: Kim, Gwanjeong
name: Kim, Mi-Ryang
name: Kim, Shinyoung
name: Kim, Jongsoo
name: Kirk, Jason
name: Kobayashi, Masato I. N.
name: Kusune, Takayoshi
name: Kwon, Jungmi
name: Lacaille, Kevin
name: Law, Chi-Yan
name: Lee, Chin-Fei
name: Lee, Yong-Hee
name: Lee, Hyeseung
name: Lee, Jeong-Eun
name: Lee, Sang-Sung
name: Li, Dalei
name: Li, Di
name: Li, Hua-bai
name: Lin, Sheng-Jun
name: Liu, Sheng-Yuan
name: Liu, Hong-Li
name: Liu, Junhao
name: Liu, Tie
name: Lu, Xing
name: Mairs, Steve
name: Matsumura, Masafumi
name: Matthews, Brenda
name: Moriarty-Schieven, Gerald
name: Nagata, Tetsuya
name: Nakamura, Fumitaka
name: Nakanishi, Hiroyuki
name: Ngoc, Nguyen Bich
name: Ohashi, Nagayoshi
name: Park, Geumsook
name: Parsons, Harriet
name: Peretto, Nicolas
name: Priestley, Felix
name: Pyo, Tae-Soo
name: Qian, Lei
name: Rao, Ramprasad
name: Rawlings, Jonathan
name: Rawlings, Mark G.
name: Retter, Brendan
name: Richer, John
name: Rigby, Andrew
name: Saito, Hiro
name: Savini, Giorgio
name: Seta, Masumichi
name: Shimajiri, Yoshito
name: Shinnaga, Hiroko
name: Tahani, Mehrnoosh
name: Tang, Ya-Wen
name: Tomisaka, Kohji
name: Tram, Le Ngoc
name: Tsukamoto, Yusuke
name: Viti, Serena
name: Wang, Hongchi
name: Wang, Jia-Wei
name: Whitworth, Anthony
name: Wu, Jintai
name: Xie, Jinjin
name: Yen, Hsi-Wei
name: Yoo, Hyunju
name: Yuan, Jinghua
name: Yun, Hyeong-Sik
name: Zenko, Tetsuya
name: Zhang, Yapeng
name: Zhang, Chuan-Peng
name: Zhang, Guoyin
name: Zhou, Jianjun
name: Zhu, Lei
name: de Looze, Ilse
name: André, Philippe
name: Dowell, C. Darren
name: Eyres, Stewart
name: Falle, Sam
name: Robitaille, Jean-François
name: van Loo, Sven
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We present 850 $μ$m polarimetric observations toward the Serpens Main molecular cloud obtained using the POL-2 polarimeter on the James Clerk Maxwell Telescope (JCMT) as part of the B-fields In STar-forming Region Observations (BISTRO) survey. These observations probe the magnetic field morphology of the Serpens Main molecular cloud on about 6000 au scales, which consists of cores and six filaments with different physical properties such as density and star formation activity. Using the histogram of relative orientation (HRO) technique, we find that magnetic fields are parallel to filaments in less dense filamentary structures where $N_{H_2} &lt; 0.93\times 10^{22}$ cm$^{-2}$ (magnetic fields perpendicular to density gradients), while being perpendicular to filaments (magnetic fields parallel to density gradients) in dense filamentary structures with star formation activity. Moreover, applying the HRO technique to denser core regions, we find that magnetic field orientations change to become perpendicular to density gradients again at $N_{H_2} \approx 4.6 \times 10^{22}$ cm$^{-2}$. This can be interpreted as a signature of core formation. At $N_{H_2} \approx 16 \times 10^{22}$ cm$^{-2}$ magnetic fields change back to being parallel to density gradients once again, which can be understood to be due to magnetic fields being dragged in by infalling material. In addition, we estimate the magnetic field strengths of the filaments ($B_{POS} = 60-300~μ$G)) using the Davis-Chandrasekhar-Fermi method and discuss whether the filaments are gravitationally unstable based on magnetic field and turbulence energy densities.
description: 18 pages, accepted for publication in ApJ