Magnetic fields towards Ophiuchus-B derived from SCUBA-2 polarization measurements
Creators: name: Soam, Archana
name: Pattle, Kate
name: Ward-Thompson, Derek
name: Lee, Chang Won
name: Sadavoy, Sarah
name: Koch, Patrick M.
name: Kim, Gwanjeong
name: Kwon, Jungmi
name: Kwon, Woojin
name: Arzoumanian, Doris
name: Berry, David
name: Hoang, Thiem
name: Tamura, Motohide
name: Lee, Sang-Sung
name: Liu, Tie
name: Kim, Kee-Tae
name: Johnstone, Doug
name: Nakamura, Fumitaka
name: Lyo, A-Ran
name: Onaka, Takashi
name: Kim, Jongsoo
name: Furuya, Ray S.
name: Hasegawa, Tetsuo
name: Lai, Shih-Ping
name: Bastien, Pierre
name: Chung, Eun Jung
name: Kim, Shinyoung
name: Parsons, Harriet
name: Rawlings, Mark
name: Mairs, Steve
name: Graves, Sarah F.
name: Robitaille, J. -F.
name: Liu, Hong-Li
name: Whitworth, Anthony P.
name: Eswaraiah, Chakali
name: Rao, Ramprasad
name: Yoo, Hyunju
name: Houde, Martin
name: Kang, Ji-hyun
name: Doi, Yasuo
name: Choi, Minho
name: Kang, Miju
name: Coude, Simon
name: Li, Hua-bai
name: Matsumura, Masafumi
name: Matthews, Brenda C.
name: Pon, Andy
name: Di Francesco, James
name: Hayashi, Saeko S.
name: Kawabata, Koji S.
name: Inutsuka, Shu-ichiro
name: Qiu, Keping
name: Franzmann, Erica
name: Friberg, Per
name: Greaves, Jane S.
name: Kirk, Jason M.
name: Li, Di
name: Shinnaga, Hiroko
name: van Loo, Sven
name: Aso, Yusuke
name: Byun, Do-Young
name: Chen, Huei-Ru
name: Chen, Mike C. -Y.
name: Chen, Wen Ping
name: Ching, Tao-Chung
name: Cho, Jungyeon
name: Chrysostomou, Antonio
name: Drabek-Maunder, Emily
name: Eyres, Stewart P. S.
name: Fiege, Jason
name: Friesen, Rachel K.
name: Fuller, Gary
name: Gledhill, Tim
name: Griffin, Matt J.
name: Gu, Qilao
name: Hatchell, Jennifer
name: Holland, Wayne
name: Inoue, Tsuyoshi
name: Iwasaki, Kazunari
name: Jeong, Il-Gyo
name: Kang, Sung-ju
name: Kemper, Francisca
name: Kim, Kyoung Hee
name: Kim, Mi-Ryang
name: Lacaille, Kevin M.
name: Lee, Jeong-Eun
name: Li, Dalei
name: Liu, Junhao
name: Liu, Sheng-Yuan
name: Moriarty-Schieven, Gerald H.
name: Nakanishi, Hiroyuki
name: Ohashi, Nagayoshi
name: Peretto, Nicolas
name: Pyo, Tae-Soo
name: Qian, Lei
name: Retter, Brendan
name: Richer, John
name: Rigby, Andrew
name: Savini, Giorgio
name: Scaife, Anna M. M.
name: Tang, Ya-Wen
name: Tomisaka, Kohji
name: Wang, Hongchi
name: Wang, Jia-Wei
name: Yen, Hsi-Wei
name: Yuan, Jinghua
name: Zhang, Chuan-Peng
name: Zhang, Guoyin
name: Zhou, Jianjun
name: Zhu, Lei
name: Andre, Philippe
name: Dowell, C. Darren
name: Falle, Sam
name: Tsukamoto, Yusuke
name: Kanamori, Yoshihiro
name: Kataoka, Akimasa
name: Kobayashi, Masato I. N.
name: Nagata, Tetsuya
name: Saito, Hiro
name: Seta, Masumichi
name: Hwang, Jihye
name: Han, Ilseung
name: Lee, Hyeseung
name: Zenko, Tetsuya
Publisher: name: arXiv
Year: 2018
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We present the results of dust emission polarization measurements of Ophiuchus-B (Oph-B) carried out using the Submillimetre Common-User Bolometer Array 2 (SCUBA-2) camera with its associated polarimeter (POL-2) on the James Clerk Maxwell Telescope (JCMT) in Hawaii. This work is part of the B-fields In Star-forming Region Observations (BISTRO) survey initiated to understand the role of magnetic fields in star formation for nearby star-forming molecular clouds. We present a first look at the geometry and strength of magnetic fields in Oph-B. The field geometry is traced over $\sim$0.2 pc, with clear detection of both of the sub-clumps of Oph-B. The field pattern appears significantly disordered in sub-clump Oph-B1. The field geometry in Oph-B2 is more ordered, with a tendency to be along the major axis of the clump, parallel to the filamentary structure within which it lies. The degree of polarization decreases systematically towards the dense core material in the two sub-clumps. The field lines in the lower density material along the periphery are smoothly joined to the large scale magnetic fields probed by NIR polarization observations. We estimated a magnetic field strength of 630$\pm$410 $μ$G in the Oph-B2 sub-clump using a Davis-Chandeasekhar-Fermi analysis. With this magnetic field strength, we find a mass-to-flux ratio $λ$= 1.6$\pm$1.1, which suggests that the Oph-B2 clump is slightly magnetically supercritical.
description: 17 pages, 10 figures, Accepted for publication in ApJ