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, D.; Kim, Gwanjeong; Hoang, Thiem; Hwang, Jihye; Liu, Sheng-Yuan; Berry, D. S.; Bastien, Pierre; Hasegawa, Tetsuo; Kwon, Woojin; Qiu, Keping; André, P.; Aso, Yusuke; Byun, Do-Young; Chen, Huei-Ru Vivien; Chen, Michael C.; Chen, Wen-Ping; Ching, Tao-Chung; Cho, Jungyeon; Choi, Minho; Chrysostomou, A.; Chung, Eun Jung; Coudé, Simon; Doi, Yasuo; Dowell, C. D.; Drabek-Maunder, E.; Duan, Hao-Yuan; Eyres, S. P. S.; Falle, S. A. E. G.; Fanciullo, Lapo; Fiege, Jason D.; 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.; Holland, W. S.; 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, F.; Kim, Jong-Soo; Kim, Kyoung Hee; Kim, Mi-Ryang; Kim, Shinyoung; Kirk, J. M.; Kobayashi, Masato I. N.; Könyves, V.; Kwon, Jungmi; Lacaille, Kevin; Lee, Hyeseung; Lee, Jeong Eun; Lee, Sang-Sung; Lee, Jun Young; Li, Dalei; Li, Di; Li, Hua-bai; Liu, Hongli; Liu, Junhao; Lyo, A-Ran; Matsumura, Masatoshi; Matthews, Brenda C.; Moriarty‐Schieven, G. H.; Nagata, T.; Nakamura, Fúmitaka; Nakanishi, Hiroyuki; Ohashi, Nagayoshi; Park, Geumsook; Parsons, Harriet; Pascale, Enzo; Peretto, N.; Pon, Andy; Pyo, Tae‐Soo; Qian, Lei; Rao, Ramprasad; Rawlings, Mark G.; Retter, Brendan; Richer, J. S.; Rigby, Andrew; Robitaille, Jean‐François; Sadavoy, Sarah; Saito, Hiro; Savini, G.; Scaife, Anna M. M.; Seta, Masumichi; Shinnaga, Hiroko; Tang, Ya-Wen; Tomisaka, Kohji; Tsukamoto, Yusuke; Loo, S. Van; Wang, Hongchi; Whitworth, Anthony Peter; Yen, Hsi-Wei; Yoo, Hyunju; Yuan, Jinghua; Yun, Hyeong-Sik; Zenko, Tetsuya; Zhang, Chuan-Peng; Zhang, Guoyin; Zhang, Yapeng; Zhou, Jianjun; Zhu, Lei

doi:10.3847/1538-4357/ab13a2

Cited by 56 publications

(62 citation statements)

References 99 publications

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“…This survey is designed to cover a variety of nearby star-forming regions, with an initial focus on the Gould Belt molecular clouds. The regions published so far are Orion A (Pattle et al 2017), M16 (Pattle et al 2018), ρ Ophiuchus A (Kwon et al 2018), ρ Ophiuchus B (Soam et al 2018), ρ Ophiuchus C (Liu et al 2019), Perseus B1 (Coudé et al 2019), and IC 5146 (Wang et al 2019). In this paper, we present new observational results of the NGC 1333 star-forming region in the Perseus molecular cloud obtained by the BISTRO survey.…”

Section: Introductionmentioning

confidence: 80%

The JCMT BISTRO Survey: Magnetic Fields Associated with a Network of Filaments in NGC 1333

Doi¹,

Hasegawa

Furuya

et al. 2020

ApJ

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We present new observations of the active star formation region NGC 1333 in the Perseus molecular cloud complex from the James Clerk Maxwell Telescope B-Fields In Star-forming Region Observations (BISTRO) survey with the POL-2 instrument. The BISTRO data cover the entire NGC 1333 complex (∼1.5 pc×2 pc) at 0.02 pc resolution and spatially resolve the polarized emission from individual filamentary structures for the first time. The inferred magnetic field structure is complex as a whole, with each individual filament aligned at different position angles relative to the local field orientation. We combine the BISTRO data with low-and high-resolution data derived from Planck and interferometers to study the multiscale magnetic field structure in this region. The magnetic field morphology drastically changes below a scale of ∼1 pc and remains continuous from the scales of filaments (∼0.1 pc) to that of protostellar envelopes (∼0.005 pc or ∼1000 au). Finally, we construct simple models in which we assume that the magnetic field is always perpendicular to the long axis of the filaments. We demonstrate that the observed variation of the relative orientation between the filament axes and the magnetic field angles are well reproduced by this model, taking into account the projection effects of the magnetic field and filaments relative to the plane of the sky. These projection effects may explain the apparent complexity of the magnetic field structure observed at the resolution of BISTRO data toward the filament network.

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Section: Introductionmentioning

confidence: 80%

The JCMT BISTRO Survey: Magnetic Fields Associated with a Network of Filaments in NGC 1333

Doi¹,

Hasegawa

Furuya

et al. 2020

ApJ

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“…It should be noted that the standard selection of polarization vectors by their signal-to-noise ratio in polarization fraction, p/δp may create bias in the recovered value of α. The sensitivity of recent observations allows the implementation of Bayesian analyses of the ǫ p -A V relationship (Wang et al, 2018), which should better inform future discussions of the limits of applicability of submillimeter polarization observations.…”

Section: Interpretation Of Polarization Fractionmentioning

confidence: 99%

Submillimeter and Far-Infrared Polarimetric Observations of Magnetic Fields in Star-Forming Regions

Pattle

Fissel

2019

Front. Astron. Space Sci.

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Observations of star-forming regions by the current and upcoming generation of submillimeter polarimeters will shed new light on the evolution of magnetic fields over the cloud-to-core size scales involved in the early stages of the star formation process. Recent wide-area and high-sensitivity polarization observations have drawn attention to the challenges of modeling magnetic field structure of star forming regions, due to variations in dust polarization properties in the interstellar medium. However, these observations also for the first time provide sufficient information to begin to break the degeneracy between polarization efficiency variations and depolarization due to magnetic field sub-beam structure, and thus to accurately infer magnetic field properties in the star-forming interstellar medium. In this article we discuss submillimeter and far-infrared polarization observations of star-forming regions made with single-dish instruments. We summarize past, present and forthcoming single-dish instrumentation, and discuss techniques which have been developed or proposed to interpret polarization observations, both in order to infer the morphology and strength of the magnetic field, and in order to determine the environments in which dust polarization observations reliably trace the magnetic field. We review recent polarimetric observations of molecular clouds, filaments, and starless and protostellar cores, and discuss how the application of the full range of modern analysis techniques to recent observations will advance our understanding of the role played by the magnetic field in the early stages of star formation.

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“…In Section 4.2, we also find a plane-of-sky amplitude B pos =120±60 μG for the magnetic field and a criticality criterion λ c =3.0±1.5. Although this magnetic field amplitude is relatively weak when compared to the fields found in high-mass star-forming regions such as OrionA (where B pos 1.0 mG; e.g., Houde et al 2009;Pattle et al 2017) or in hub-filament structures such as IC5146 (with B pos ∼0.5 mG; e.g., Wang et al 2019), it is either comparable to or larger than the field strengths (B pos 100 μG) typically found in low-mass prestellar cores (e.g., Crutcher et al 2004;Kirk et al 2006;Liu et al 2019). Above all, these results indicate that Perseus B1 is a supercritical molecular cloud (i.e., magnetic pressure alone cannot support the cloud against gravity).…”

Section: Magnetic and Turbulent Propertiesmentioning

confidence: 80%

The JCMT BISTRO Survey: The Magnetic Field of the Barnard 1 Star-forming Region

Coudé¹,

Bastien²,

Houde³

et al. 2019

ApJ

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We present the POL-2 850 μm linear polarization map of the Barnard1 clump in the Perseus molecular cloud complex from the B-fields In STar-forming Region Observations survey at the James Clerk Maxwell Telescope. We find a trend of decreasing polarization fraction as a function of total intensity, which we link to depolarization effects toward higher-density regions of the cloud. We then use the polarization data at 850 μm to infer the planeof-sky orientation of the large-scale magnetic field in Barnard1. This magnetic field runs north-south across most of the cloud, with the exception of B1-c, where it turns more east-west. From the dispersion of polarization angles, we calculate a turbulence correlation length of 5.0±2 5 (1500 au) and a turbulent-to-total magnetic energy ratio of 0.5±0.3 inside the cloud. We combine this turbulent-to-total magnetic energy ratio with observations of NH 3 molecular lines from the Green Bank Ammonia Survey to estimate the strength of the plane-of-sky component of the magnetic field through the Davis-Chandrasekhar-Fermi method. With a plane-of-sky amplitude of 120±60 μG and a criticality criterion λ c =3.0±1.5, we find that Barnard1 is a supercritical molecular cloud with a magnetic field nearly dominated by its turbulent component.

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

Cited by 56 publications

References 99 publications

The JCMT BISTRO Survey: Magnetic Fields Associated with a Network of Filaments in NGC 1333

The JCMT BISTRO Survey: Magnetic Fields Associated with a Network of Filaments in NGC 1333

Submillimeter and Far-Infrared Polarimetric Observations of Magnetic Fields in Star-Forming Regions

The JCMT BISTRO Survey: The Magnetic Field of the Barnard 1 Star-forming Region

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