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

Coudé, Simon; Bastien, Pierre; Houde, Martin; Sadavoy, Sarah; Friesen, Rachel; Francesco, James Di; Johnstone, Doug; Mairs, Steve; Hasegawa, Tetsuo; Kwon, Woojin; Lai, Shih-Ping; Qiu, Keping; Ward-Thompson, Derek; Berry, D. S.; Chen, Michael Chun-Yuan; Fiege, Jason D.; Franzmann, Erica; Hatchell, Jennifer; Lacaille, Kevin; Matthews, Brenda C.; Moriarty‐Schieven, G. H.; Pon, Andy; André, P.; Arzoumanian, D.; Aso, Yusuke; Byun, Doyoung; Eswaraiah, Chakali; Chen, Huei-Ru Vivien; Chen, Wen-Ping; Ching, Tao-Chung; Cho, Jungyeon; Choi, Minho; Chrysostomou, A.; Chung, Eun Jung; Doi, Yasuo; Drabek-Maunder, E.; Dowell, C. D.; Eyres, S. P. S.; Falle, S. A. E. G.; Friberg, Per; Fuller, G. A.; Furuya, Ray S.; Gledhill, Tim; Graves, Sarah; Greaves, J. S.; Griffin, Matt; Gu, Qilao; Hayashi, Saeko S.; Hoang, Thiem; Holland, W. S.; Inoue, Tsuyoshi; Inutsuka, Shu‐ichiro; Iwasaki, Kazunari; Jeong, Il-Gyo; Kanamori, Yoshihiro; Kataoka, Akimasa; Kang, Ji-hyun; Kang, Miju; Kang, Sung-Ju; Kawabata, Koji S.; Kemper, F.; Kim, Gwanjeong; Kim, Jong-Soo; Kim, Kee‐Tae; Kim, Kyoung Hee; Kim, Mi-Ryang; Kim, Shinyoung; Kirk, J. M.; Kobayashi, Masato I. N.; Koch, Patrick M.; Kwon, Jungmi; Lee, Jeong Eun; Lee, Chang Won; Lee, Sang-Sung; Li, Dalei; Li, Di; Li, Hua-bai; Liu, Hongli; Liu, Junhao; Liu, Sheng-Yuan; Li, Shipeng; Loo, S. Van; Lyo, A-Ran; Matsumura, Masatoshi; Nagata, T.; Nakamura, Fúmitaka; Nakanishi, Hiroyuki; Ohashi, Nagayoshi; Onaka, Takashi; Parsons, Harriet; Pattle, Kate; Peretto, N.; Pyo, Tae‐Soo; Qian, Lei; Rao, Ramprasad; Rawlings, Mark G.; Retter, Brendan; Richer, J. S.; Rigby, Andrew; Robitaille, Jean‐François; Saito, Hiro; Savini, G.; Scaife, Anna M. M.; Seta, Masumichi; Shinnaga, Hiroko; Soam, Archana; Tamura, Motohide; Tang, Ya-Wen; Tomisaka, Kohji; Tsukamoto, Yusuke; Wang, Hongchi; Wang, Jiawei; Whitworth, Anthony Peter; Yen, Hsi-Wei; Yoo, Hyunju; Yuan, Jinghua; Zenko, Tetsuya; Zhang, Chuan-Peng; Zhang, Guoyin; Zhou, Jianjun; Zhu, Lei

doi:10.3847/1538-4357/ab1b23

Cited by 43 publications

(32 citation statements)

References 107 publications

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“…Due to the limited number of data-points available for the fit, we fix the turbulence correlation scale on δ = 20 mpc. This value is in good agreement with previous estimation of this quantity in other star forming regions: for instance Houde et al (2009) found δ = 16 mpc in OMC-1, Frau et al (2014) derived δ = 13−33 mpc in the high-mass star forming region NGC 7538, and Coudé et al (2019) reported δ = 7 mpc in Barnard 1. Furthermore, we assume the cloud thickness ∆ to be equal to the source effective radius (r eff ), defined as the radius of a circular region of identical surface area.…”

Section: Angular Dispersion Function and Field Strengthsupporting

confidence: 92%

“…The first assumption regards the turbulence correlation scale, δ. The literature results seem to suggest that δ is lower for low-mass starforming regions, with respect to high-mass ones: both Liu et al (2019) and Coudé et al (2019) found δ < 10 mpc in low-mass cores. We therefore tested other 3 values (5, 10, 15 mpc), obtaining B pos = 16, 40, 62 µG respectively.…”

Section: Influence Of the Assumed Parametersmentioning

confidence: 95%

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Magnetic properties of the protostellar core IRAS 15398-3359

Redaelli

Alves

Santos

et al. 2019

A&A

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Context. Magnetic fields can affect significantly the star formation process. The theory of the magnetically-driven collapse in a uniform field predicts that initially the contraction happens along the field lines. When the gravitational pull grows strong enough, the magnetic field lines pinch inwards, giving rise to a characteristic hourglass shape. Aims. We investigate the magnetic field structure of a young Class 0 object, IRAS 15398-3359, embedded in the Lupus I cloud. Previous observations at large scales suggest that this source evolved in an highly magnetised environment. This object thus appears an ideal candidate to study the magnetically driven core collapse in the low-mass regime. Methods. We have performed polarisation observations of IRAS 15398-3359 at 214 µm using the SOFIA/HAWC+ instrument, thus tracing the linearly polarised thermal emission of cold dust. Results. Our data unveil a significant bend of the magnetic field lines due to the gravitational pull. The magnetic field appears ordered and aligned with the large-scale B-field of the cloud and with the outflow direction. We estimate a magnetic field strength of B = 78 µG, expected to be accurate within a factor of two. The measured mass-to-flux parameter is λ = 0.95, indicating that the core is in a transcritical regime.

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Section: Angular Dispersion Function and Field Strengthsupporting

confidence: 92%

Section: Influence Of the Assumed Parametersmentioning

confidence: 95%

Magnetic properties of the protostellar core IRAS 15398-3359

Redaelli

Alves

Santos

et al. 2019

A&A

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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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“…For σ PI , we use the mean rms from the Stokes Q and U observations, taking into account that the map sensitivities vary across the primary beam. The polarization position angle, θ, and its uncertainty σ θ are given by (e.g., Coudé et al 2019),…”

Section: Debias Correctionmentioning

confidence: 99%

Dust Polarization toward Embedded Protostars in Ophiuchus with ALMA. III. Survey Overview

Sadavoy

Stephens

Myers

et al. 2019

ApJS

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We present 0.25 resolution (35 au) ALMA 1.3 mm dust polarization observations for 37 young stellar objects (YSOs) in the Ophiuchus molecular cloud. These data encompass all the embedded protostars in the cloud and several Flat and Class II objects to produce the largest, homogeneous study of dust polarization on disk scales to date. The goal of this study is to study dust polarization morphologies down to disk scales. We find that 14/37 (38%) of the observed YSOs are detected in polarization at our sensitivity. Nine of these sources have uniform polarization angles and four sources have azimuthal polarization structure. We find that the sources with uniform polarization tend to have steeper inclinations (> 60 • ) than those with azimuthal polarization (< 60 • ). Overall, the majority (9/14) of the detected sources have polarization morphologies and disk properties consistent with dust self-scattering processes in optically thick disks. The remaining sources may be instead tracing magnetic fields. Their inferred field directions from rotating the polarization vectors by 90 • are mainly poloidal or hourglass shaped. We find no evidence of a strong toroidal field component toward any of our disks. For the 23 YSOs that are undetected in polarization, roughly half of them have 3-sigma upper limits of < 2%. These sources also tend to have inclinations < 60 • and they are generally compact. Since lower inclination sources tend to have azimuthal polarization, these YSOs may be undetected in polarization due to unresolved polarization structure within our beam. We propose that disks with inclinations > 60 • are the best candidates for future polarization studies of dust selfscattering as these systems will generally show uniform polarization vectors that do not require very high resolution to resolve. We release the continuum and polarization images for all the sources with this publication. Data from the entire survey can be obtained from Dataverse. † Hubble Fellow

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

Cited by 43 publications

References 107 publications

Magnetic properties of the protostellar core IRAS 15398-3359

Magnetic properties of the protostellar core IRAS 15398-3359

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

Dust Polarization toward Embedded Protostars in Ophiuchus with ALMA. III. Survey Overview

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