The JCMT BISTRO Survey: Revealing the Diverse Magnetic Field Morphologies in Taurus Dense Cores with Sensitive Submillimeter Polarimetry

Eswaraiah, Chakali; Li, Di; Furuya, Ray S.; Hasegawa, Tetsuo; Ward-Thompson, Derek; Qiu, Keping; Ohashi, Nagayoshi; Pattle, Kate; Sadavoy, Sarah; Hull, Charles L. H.; Berry, D. S.; Doi, Yasuo; Ching, Tao-Chung; Lai, Shih-Ping; Wang, Jiawei; Koch, Patrick M.; Kwon, Jungmi; Kwon, Woojin; Bastien, Pierre; Arzoumanian, D.; Coudé, Simon; Soam, Archana; Fanciullo, Lapo; Yen, Hsi-Wei; Liu, Junhao; Hoang, Thiem; Chen, Wen-Ping; Shimajiri, Yoshito; Li, Shipeng; Chen, Zhiwei; Li, Hua-bai; Lyo, A-Ran; Hwang, Jihye; Johnstone, Doug; Rao, Ramprasad; Ngoc, Nguyen Bich; Diep, P. N.; Mairs, Steve; Parsons, Harriet; Tamura, Motohide; Tahani, Mehrnoosh; Chen, Huei-Ru Vivien; Nakamura, Fúmitaka; Shinnaga, Hiroko; Tang, Ya-Wen; Cho, Jungyeon; Lee, Chang Won; Inutsuka, Shu‐ichiro; Inoue, Tsuyoshi; Iwasaki, Kazunari; Qian, Lei; Xie, Jinjin; Li, Dalei; Liu, Hongli; Zhang, Chuan-Peng; Chen, Mike Y.; Zhang, Guoyin; Zhu, Lei; Zhou, Jianjun; André, P.; Liu, Sheng-Yuan; Yuan, Jinghua; Lu, Xing; Peretto, N.; Bourke, Tyler L.; Byun, Doyoung; Dai, Sophia; Duan, Yan; Duan, Hao-Yuan; Eden, David; Matthews, Brenda C.; Fiege, Jason D.; Fissel, Laura M.; Kim, Kee‐Tae; Lee, Chin-Fei; Kim, Jong-Soo; Pyo, Tae‐Soo; Choi, Yunhee; Choi, Minho; Chrysostomou, A.; Chung, Eun Jung; Tram, Le Ngoc; Franzmann, Erica; Friberg, Per; Friesen, Rachel; Fuller, G. A.; Gledhill, Tim; Graves, Sarah; Greaves, J. S.; Griffin, Matt; Gu, Qilao; Han, Ilseung; Hatchell, Jennifer; Hayashi, Saeko S.; Houde, Martin; Kawabata, Koji S.; Jeong, Il-Gyo; Kang, Ji-hyun; Kang, Sung-Ju; Kang, Miju; Kataoka, Akimasa; Kemper, F.; Rawlings, Mark G.; Rawlings, J. M. C.; Retter, Brendan; Richer, J. S.; Rigby, Andrew; Saito, Hiro; Savini, G.; Scaife, Anna M. M.; Seta, Masumichi; Kim, Gwanjeong; Kim, Kyoung Hee; Kim, Mi-Ryang; Kirchschlager, Florian; Kirk, J. M.; Kobayashi, Masato I. N.; Könyves, V.; Kusune, Takayoshi; Lacaille, Kevin; Law, Chi-Yan; Lee, Sang-Sung; Lee, Jun Young; Matsumura, Masatoshi; Moriarty‐Schieven, G. H.; Nagata, T.; Nakanishi, Hiroyuki; Onaka, Takashi; Park, Geumsook; Tang, Xindi; Tomisaka, Kohji; Tsukamoto, Yusuke; Viti, S.; Wang, Hongchi; Whitworth, Anthony Peter; Yoo, Hyunju; Yun, Hyeong-Sik; Zenko, Tetsuya; Zhang, Yapeng; Looze, I. De; Dowell, C. D.; Eyres, S. P. S.; Falle, S. A. E. G.; Robitaille, Jean‐François; Loo, S. Van

doi:10.3847/2041-8213/abeb1c

Cited by 26 publications

(19 citation statements)

References 96 publications

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“…However, the hourglass morphology of the magnetic fields is frequently found in massive star-forming clouds, indicating that the magnetic field can be modified by gravity or outflows in subparsec scales (e.g., Wang et al 2019;Lyo et al 2021). Besides, the shocks from outflows, stellar feedback of expanding ionization fronts of H II region, and gas flow driven by gravity are considered to cause the magnetic field distortions (e.g., Hull et al 2017;Pillai et al 2020;Arzoumanian et al 2021;Eswaraiah et al 2021). Hence, the significance of magnetic field may change from time to time as well as from cloud to cloud.…”

Section: Introductionmentioning

confidence: 99%

Evolution of the Hub-filament Structures in IC 5146 in the Context of the Energy Balance of Gravity, Turbulence, and Magnetic Field

Chung

Lee

Kwon

et al. 2022

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We present the results of 850 μm polarization and C18O (3 − 2) line observations toward the western hub-filament structure (W-HFS) of the dark Streamer in IC 5146 using the James Clerk Maxwell Telescope SCUBA-2/POL-2 and HARP instruments. We aim to investigate how the relative importance of the magnetic field, gravity, and turbulence affects core formation in HFS by comparing the energy budget of this region. We identified four 850 μm cores and estimated the magnetic field strengths (B pos) of the cores and the hub and filament using the Davis–Chandrasekhar–Fermi method. The estimated B pos is ∼80 to 1200 μG. From Wang et al., B pos of E-47, a core in the eastern hub (E-hub), and E-hub were reestimated to be 500 and 320 μG, respectively, with the same method. We measured the gravitational (E G), kinematic (E K), and magnetic energies (E B) in the filament and hubs and compared the relative importance among them. We found that an E B-dominant filament has aligned fragmentation type, while E G-dominant hubs show no and clustered fragmentation types. In the E G dominant hubs, it seems that the portion of E K determines whether the hub becomes to have clustered (the portion of E K ∼ 20%) or no fragmentation type (∼10%). We propose an evolutionary scenario for the E- and W-HFSs, where the HFS forms first by the collision of turbulent flows, and then the hubs and filaments can go into various types of fragmentation depending on their energy balance of gravity, turbulence, and magnetic field.

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Section: Introductionmentioning

confidence: 99%

Evolution of the Hub-filament Structures in IC 5146 in the Context of the Energy Balance of Gravity, Turbulence, and Magnetic Field

Chung

Lee

Kwon

et al. 2022

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“…High angular resolution observations at (sub-)millimeter wavelengths show that the thermal dust emission probing the envelope-to-disk scales (~50-10,000 au) is polarized at a few percent level. This has been observed both in low and high mass star-forming regions (Matthews et al, 2009;Zhang et al, 2014;Galametz et al, 2018;Hull and Zhang, 2019;Beltrán et al, 2019;Sanhueza et al, 2021;Eswaraiah et al, 2021). Considering that the polarized flux is a quantity that is prone to cancellation if the polarization angle is highly disorganized along the line-of-sight, observations of rather large polarization fractions suggest the magnetic field lines underlying the alignment of the protostellar dust remain at least partly organized inside star-forming cores (Le .…”

Section: Magnetic Fields At Core's Scalesmentioning

confidence: 90%

Recent progress with observations and models to characterize the magnetic fields from star-forming cores to protostellar disks

Maury

Hennebelle

Girart

2022

Front. Astron. Space Sci.

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In this review article, we aim at providing a global outlook on the progresses made in the recent years to characterize the role of magnetic fields during the embedded phases of the star formation process. Thanks to the development of observational capabilities and the parallel progress in numerical models, capturing most of the important physics at work during star formation; it has recently become possible to confront detailed predictions of magnetized models to observational properties of the youngest protostars. We provide an overview of the most important consequences when adding magnetic fields to state-of-the-art models of protostellar formation, emphasizing their role to shape the resulting star(s) and their disk(s). We discuss the importance of magnetic field coupling to set the efficiency of magnetic processes and provide a review of observational works putting constraints on the two main agents responsible for the coupling in star-forming cores: dust grains and ionized gas. We recall the physical processes and observational methods, which allow to trace the magnetic field topology and its intensity in embedded protostars and review the main steps, success, and limitations in comparing real observations to synthetic observations from the non-ideal MHD models. Finally, we discuss the main threads of observational evidence that suggest a key role of magnetic fields for star and disk formation, and propose a scenario solving the angular momentum for star formation, also highlighting the remaining tensions that exist between models and observations.

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“…Numerous observatories, including the James Clark Maxwell Telescope (JCMT; e.g., Eswaraiah et al, 2021;Ngoc et al, 2021;Hwang et al, 2021;Kwon et al, 2022), Planck Space Observatory (e.g., Planck Collaboration et al, 2016;Alina et al, 2019), Atacama Large Millimeter/sub-millimeter Array (ALMA; e.g., Pattle et al, 2021;Cortés et al, 2021), Sub-Millimeter Array (SMA; e.g., Zhang et al, 2014), and Stratospheric Observatory for Infrared Astronomy (SOFIA; e.g., Chuss et al, 2019) have observed B POS of numerous star-forming regions. However, the number of B LOS observations of molecular clouds are still limited.…”

Section: D Magnetic Fieldsmentioning

confidence: 99%

Three-dimensional magnetic fields of molecular clouds

Tahani

2022

Front. Astron. Space Sci.

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To investigate the role of magnetic fields in the evolution of the interstellar medium, formation and evolution of molecular clouds, and ultimately the formation of stars, their three-dimensional (3D) magnetic fields must be probed. Observing only one component of magnetic fields (along the line of sight or parallel to the plane of the sky) is insufficient to identify these 3D vectors. In recent years, novel techniques for probing each of these two components and integrating them with additional data (from observations or models), such as Galactic magnetic fields or magnetic field inclination angles, have been developed, in order to infer 3D magnetic fields. We review and discuss these advancements, their applications, and their future direction.

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The JCMT BISTRO Survey: Revealing the Diverse Magnetic Field Morphologies in Taurus Dense Cores with Sensitive Submillimeter Polarimetry

Cited by 26 publications

References 96 publications

Evolution of the Hub-filament Structures in IC 5146 in the Context of the Energy Balance of Gravity, Turbulence, and Magnetic Field

Evolution of the Hub-filament Structures in IC 5146 in the Context of the Energy Balance of Gravity, Turbulence, and Magnetic Field

Recent progress with observations and models to characterize the magnetic fields from star-forming cores to protostellar disks

Three-dimensional magnetic fields of molecular clouds

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