JCMT BISTRO Observations: Magnetic Field Morphology of Bubbles Associated with NGC 6334

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

doi:10.3847/1538-4357/acac81

Cited by 6 publications

(3 citation statements)

References 120 publications

(171 reference statements)

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“…While we adapted this decomposition and applied it to the B-fields of spiral galaxies, our method can also be applied to any vector field where a circle or ellipse is a geometry of particular interest. Apart from galaxies, this method could also be adapted to other ISM morphologies, such as supernova remnants or windblown bubbles in star-forming regions (e.g., Tahani et al 2023), or radio synchrotron loops (e.g., Vidal et al 2015).…”

Section: Broader Applicationsmentioning

confidence: 99%

The Structure of Magnetic Fields in Spiral Galaxies: A Radio and Far-infrared Polarimetric Analysis

Surgent,

Lopez-Rodriguez,

Clark

2023

ApJ

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We propose and apply a method to quantify the morphology of the large-scale ordered magnetic fields (B-fields) in galaxies. This method is adapted from the analysis of Event Horizon Telescope polarization data. We compute a linear decomposition of the azimuthal modes of the polarization field in radial galactocentric bins. We apply this approach to five low-inclination spiral galaxies with both far-infrared (FIR: 154 μm) dust polarimetric observations taken from the Survey of Extragalactic Magnetism with SOFIA (SALSA) and radio (6 cm) synchrotron polarization observations. We find that the main contribution to the B-field structure of these spiral galaxies comes from the m = 2 and m = 0 modes at FIR wavelengths and the m = 2 mode at radio wavelengths. The m = 2 mode has a spiral structure and is directly related to the magnetic pitch angle, while m = 0 has a constant B-field orientation. The FIR data tend to have a higher relative contribution from other modes than the radio data. The extreme case is NGC 6946: all modes contribute similarly in the FIR, while m = 2 still dominates in the radio. The average magnetic pitch angle in the FIR data is smaller and has greater angular dispersion than in the radio, indicating that the B-fields in the disk midplane traced by FIR dust polarization are more tightly wound and more chaotic than the B-field structure in the radio, which probes a larger volume. We argue that our approach is more flexible and model independent than standard techniques, while still producing consistent results where directly comparable.

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Section: Broader Applicationsmentioning

confidence: 99%

The Structure of Magnetic Fields in Spiral Galaxies: A Radio and Far-infrared Polarimetric Analysis

Surgent,

Lopez-Rodriguez,

Clark

2023

ApJ

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“…as defined by Tahani et al (2023) and shown in Figure 3 for the HAWC+ 53 μm (upper left panel), HAWC+ 154 μm (upper right panel), and the JCMT POL-2 850 μm observations (lower panel). The data have the same constraints of S/N(I) > 20 and S/N(P) > 2.5.…”

Section: Radial Coordinate Polarizationmentioning

confidence: 99%

Submillimeter-wavelength Polarimetry of IRC+10216

Andersson,

Karoly,

Bastien

et al. 2024

ApJ

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We present SCUBA-2/POL-2 850 μm polarimetric observations of the circumstellar envelope (CSE) of the carbon-rich asymptotic giant branch (AGB) star IRC+10216. Both far-IR (FIR) and optical polarization data indicate grains aligned with their long axis in the radial direction relative to the central star. The 850 μm polarization does not show this simple structure. The 850 μm data are indicative, albeit not conclusive, of a magnetic dipole geometry. Assuming such a simple dipole geometry, the resulting 850 μm polarization geometry is consistent with both Zeeman observations and small-scale structure in the CSE. While there is significant spectral-line polarization contained within the SCUBA-2 850 μm passband for the source, it is unlikely that our broadband polarization results are dominated by line polarization. To explain the required grain alignment, grain mineralogy effects, due to either fossil silicate grains from the earlier oxygen-rich AGB phase of the star or due to the incorporation of ferromagnetic inclusions in the largest grains, may play a role. We argue that the most likely explanation is due to a new alignment mechanism wherein a charged grain, moving relative to the magnetic field, precesses around the induced electric field and therefore aligns with the magnetic field. This mechanism is particularly attractive as the optical, FIR, and submillimeter-wave polarization of the carbon dust can then be explained in a consistent way, differing simply due to the charge state of the grains.

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“…Therefore, magnetic fields are believed to introduce anisotropy in the gas motion and consequently have a significant impact on structure formation and evolution in the ISM, ranging from galaxy formation to the formation of filamentary molecular clouds within a single star-forming region (Heiles & Crutcher 2005;Boulanger et al 2018). Indeed, magnetic field lines are expected to be influenced by the motion of the ISM, leading to their dragging or bending (e.g., Doi et al 2021a;Tahani 2022;Tahani et al 2023). As a result, the interstellar magnetic field structure is expected to be inscribed with a history of the deformation of the ISM (Gómez et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Tomographic Imaging of the Sagittarius Spiral Arm's Magnetic Field Structure

Doi 土井,

Nakamura 中村,

Kawabata 川端

et al. 2024

ApJ

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The Galactic global magnetic field is thought to play a vital role in shaping Galactic structures such as spiral arms and giant molecular clouds. However, our knowledge of magnetic field structures in the Galactic plane at different distances is limited, as measurements used to map the magnetic field are the integrated effect along the line of sight. In this study, we present the first ever tomographic imaging of magnetic field structures in a Galactic spiral arm. Using optical stellar polarimetry over a 17 ′ × 10 ′ field of view, we probe the Sagittarius spiral arm. Combining these data with stellar distances from the Gaia mission, we can isolate the contributions of five individual clouds along the line of sight by analyzing the polarimetry data as a function of distance. The observed clouds include a foreground cloud (d < 200 pc) and four clouds in the Sagittarius arm at 1.23, 1.47, 1.63, and 2.23 kpc. The column densities of these clouds range from 0.5 to 2.8 × 1021 cm−2. The magnetic fields associated with each cloud show smooth spatial distributions within their observed regions on scales smaller than 10 pc and display distinct orientations. The position angles projected on the plane of the sky, measured from the Galactic north to the east, for the clouds in increasing order of distance are 135°, 46°, 58°, 150°, and 40°, with uncertainties of a few degrees. Notably, these position angles deviate significantly from the direction parallel to the Galactic plane.

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JCMT BISTRO Observations: Magnetic Field Morphology of Bubbles Associated with NGC 6334

Cited by 6 publications

References 120 publications

The Structure of Magnetic Fields in Spiral Galaxies: A Radio and Far-infrared Polarimetric Analysis

The Structure of Magnetic Fields in Spiral Galaxies: A Radio and Far-infrared Polarimetric Analysis

Submillimeter-wavelength Polarimetry of IRC+10216

Tomographic Imaging of the Sagittarius Spiral Arm's Magnetic Field Structure

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