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B-fields in Star-forming Region Observations (BISTRO): Magnetic Fields in the Filamentary Structures of Serpens Main
Kwon, Woojin1,2; Pattle, Kate3,4; Sadavoy, Sarah5; Hull, Charles L. H.6,7; Johnstone, Doug8,9; Ward-Thompson, Derek10; Di Francesco, James8,9; Koch, Patrick M.11; Furuya, Ray12,13; Doi, Yasuo14; Le Gouellec, Valentin J. M.15,16; Hwang, Jihye17,18; Lyo, A-Ran17; Soam, Archana15,19; Tang, Xindi20; Hoang, Thiem17,18; Kirchschlager, Florian3; Eswaraiah, Chakali21,22; Fanciullo, Lapo11; Kim, Kyoung Hee17; Onaka, Takashi23,24; Konyves, Vera10; Kang, Ji-hyun17; Lee, Chang Won17,18; Tamura, Motohide24,25,26; Bastien, Pierre27,28; Hasegawa, Tetsuo26; Lai, Shih-Ping11,29,30; Qiu, Keping31,32; Berry, David33; Arzoumanian, Doris34; Bourke, Tyler L.35,36; Byun, Do-Young17,18; Chen, Wen Ping37; Chen, Huei-Ru Vivien17; Chen, Mike11,29,30; Chen, Zhiwei9; Ching, Tao-Chung38; Cho, Jungyeon21,39; Choi, Yunhee40; Choi, Minho17; Chrysostomou, Antonio35; Chung, Eun Jung40; Coude, Simon15; Dai, Sophia39; Pham Ngoc Diep41; Duan, Yan39; Hao-Yuan Duan29,30; Eden, David42; Fiege, Jason43; Fissel, Laura M.5; Franzmann, Erica43; Friberg, Per33; Friesen, Rachel44; Fuller, Gary36; Gledhill, Tim45; Graves, Sarah33; Greaves, Jane46; Griffin, Matt46; Gu, Qilao47; Han, Ilseung17,18; Hatchell, Jennifer48; Hayashi, Saeko49; Houde, Martin50; Inoue, Tsuyoshi51; Inutsuka, Shu-ichiro51; Iwasaki, Kazunari52; Jeong, Il-Gyo17,53; Kang, Miju17; Karoly, Janik10; Kataoka, Akimasa54; Kawabata, Koji55,56,57; Kemper, Francisca11,58; Kim, Kee-Tae17,18; Kim, Gwanjeong59; Kim, Mi-Ryang17; Kim, Shinyoung17,18; Kim, Jongsoo17,18; Kirk, Jason10; Kobayashi, Masato I. N.60; Kusune, Takayoshi60; Kwon, Jungmi24; Lacaille, Kevin61,62; Law, Chi-Yan47,63; Lee, Chin-Fei11; Lee, Yong-Hee33,64; Lee, Hyeseung40; Lee, Jeong-Eun64; Lee, Sang-Sung17,18; Li, Dalei20; Li, Di21,65; Li, Hua-bai47; Lin, Sheng-Jun29,30; Liu, Sheng-Yuan11; Liu, Hong-Li66; Liu, Junhao33; Liu, Tie67; Lu, Xing68; Mairs, Steve33; Matsumura, Masafumi69,70; Matthews, Brenda8,9; Moriarty-Schieven, Gerald8; Nagata, Tetsuya71; Nakamura, Fumitaka54,72; Nakanishi, Hiroyuki73; Ngoc, Nguyen Bich41,74; Ohashi, Nagayoshi11; Park, Geumsook17; Parsons, Harriet33; Peretto, Nicolas46; Priestley, Felix46; Pyo, Tae-Soo49,72; Qian, Lei21; Rao, Ramprasad11; Rawlings, Jonathan; Rawlings, Mark G.33,75; Retter, Brendan46; Richer, John76,77; Rigby, Andrew46; Saito, Hiro78; Savini, Giorgio79; Seta, Masumichi80; Shimajiri, Yoshito26; Shinnaga, Hiroko73; Tahani, Mehrnoosh81; Tang, Ya-Wen11; Tomisaka, Kohji54,72; Le Ngoc Tram82; Tsukamoto, Yusuke73; Viti, Serena83; Wang, Hongchi38; Wang, Jia-Wei11; Whitworth, Anthony46; Wu, Jintai31; Xie, Jinjin39; Yen, Hsi-Wei11; Yoo, Hyunju17; Yuan, Jinghua39; Yun, Hyeong-Sik64; Zenko, Tetsuya71; Zhang, Yapeng84; Zhang, Chuan-Peng21,39; Zhang, Guoyin39; Zhou, Jianjun20; Zhu, Lei21; de Looze, Ilse83; Andre, Philippe85; Dowell, C. Darren86; Eyres, Stewart87; Falle, Sam88; Robitaille, Jean-Francois89; van Loo, Sven90
2022-02-01
Source PublicationASTROPHYSICAL JOURNAL
ISSN0004-637X
Volume926Issue:2Pages:13
AbstractWe present 850 mu m polarimetric observations toward the Serpens Main molecular cloud obtained using the POL-2 polarimeter on the James Clerk Maxwell Telescope as part of the B-fields In STar-forming Region Observations survey. These observations probe the magnetic field morphology of the Serpens Main molecular cloud on about 6000 au scales, which consists of cores and six filaments with different physical properties such as density and star formation activity. Using the histogram of relative orientation (HRO) technique, we find that magnetic fields are parallel to filaments in less-dense filamentary structures where NH2 < 0.93 x 10(22) cm(-2) (magnetic fields perpendicular to density gradients), while they are perpendicular to filaments (magnetic fields parallel to density gradients) in dense filamentary structures with star formation activity. Moreover, applying the HRO technique to denser core regions, we find that magnetic field orientations change to become perpendicular to density gradients again at NH2 approximate to 4.6 x 10(22) NH2 approximate to 16 x 10(22) cm(-2), magnetic fields change back to being parallel to density gradients once again, which can be understood to be due to magnetic fields being dragged in by infalling material. In addition, we estimate the magnetic field strengths of the filaments (B-POS = 60-300 mu G)) using the Davis-Chandrasekhar-Fermi method and discuss whether the filaments are gravitationally unstable based on magnetic field and turbulence energy densities.
Corresponding AuthorKwon, Woojin(wkwon@snu.ac.kr)
DOI10.3847/1538-4357/ac4bbe
Indexed BySCI ; SCI
Language英语
WOS KeywordIMAGING POLARIMETRY ; INTERSTELLAR CLOUDS ; SCUBA-2 ; POLARIZATION ; SPITZER ; LEGACY ; ORION ; 1ST ; STRENGTHS ; ALIGNMENT
Funding ProjectNational Key R&D Program of China[2017YFA0402700] ; National Key R&D Program of China[2017YFA0402600] ; Science and Technology Facilities Council of the United Kingdom ; Canada Foundation for Innovation ; New Faculty Startup Fund from Seoul National University ; National Research Foundation of Korea (NRF) - Korean government (MSIT)[NRF-2021R1F1A1061794] ; NRC Canada ; NSERC ; NAOJ Fellowship ; JSPS KAKENHI[18K13586] ; JSPS KAKENHI[20K14527] ; JSPS KAKENHI[18H05442] ; JSPS KAKENHI[15H02063] ; JSPS KAKENHI[22000005] ; National Natural Science Foundation of China (NSFC) grant[U1731237] ; Basic Science Research Program through the NRF - Ministry of Education, Science and Technology[NRF-2019R1A2C1010851] ; Science and Engineering Research Board (SERB), Department of Science and Technology (DST), Govt. of India[RJF/2020/000071] ; Ministry of Science and Technology of Taiwan[AS-IA-106-M03] ; Ministry of Science and Technology of Taiwan[106-2119-M-007-021-MY3] ; Ministry of Science and Technology of Taiwan[109-2112-M-007-010-MY3] ; Basic Science Research Program through the National Research Foundation of Korea (NRF) - Ministry of Education[NRF-2020R1A6A3A01100208] ; National Research Foundation of Korea (NRF) grant - Korean government (MSIT) through the Mid-career Research Program[2019R1A2C1087045] ; [M16AL004] ; [URF\R1\211322] ; [MOST 108-2112-M-001-004-MY2]
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000759830000001
PublisherIOP Publishing Ltd
Funding OrganizationNational Key R&D Program of China ; Science and Technology Facilities Council of the United Kingdom ; Canada Foundation for Innovation ; New Faculty Startup Fund from Seoul National University ; National Research Foundation of Korea (NRF) - Korean government (MSIT) ; NRC Canada ; NSERC ; NAOJ Fellowship ; JSPS KAKENHI ; National Natural Science Foundation of China (NSFC) grant ; Basic Science Research Program through the NRF - Ministry of Education, Science and Technology ; Science and Engineering Research Board (SERB), Department of Science and Technology (DST), Govt. of India ; Ministry of Science and Technology of Taiwan ; Basic Science Research Program through the National Research Foundation of Korea (NRF) - Ministry of Education ; National Research Foundation of Korea (NRF) grant - Korean government (MSIT) through the Mid-career Research Program
Citation statistics
Document Type期刊论文
Identifierhttp://ir.xao.ac.cn/handle/45760611-7/4508
Collection射电天文研究室_恒星形成与演化研究团组
Corresponding AuthorKwon, Woojin
Affiliation1.Seoul Natl Univ, Dept Earth Sci Educ, 1 Gwanak Ro, Seoul 08826, South Korea
2.Seoul Natl Univ, SNU Astron Res Ctr, 1 Gwanak Ro, Seoul 08826, South Korea
3.UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England
4.Natl Univ Ireland Galway, Ctr Astron, Sch Phys, Univ Rd, Galway H91 TK33, Ireland
5.Queens Univ, Dept Phys, Engn Phys & Astrophys, Kingston, ON K7L 3N6, Canada
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9.Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 2Y2, Canada
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29.Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan
30.Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan
31.Nanjing Univ, Sch Astron & Space Sci, 163 Xianlin Ave, Nanjing 210023, Peoples R China
32.Nanjing Univ, Minist Educ, Key Lab Modern Astron & Astrophys, Nanjing 210023, Peoples R China
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34.Aix Marseille Univ, LAM, CNES, CNRS, Marseille, France
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69.Kagawa Univ, Fac Educ, Saiwai Cho 1-1, Takamatsu, Kagawa 7608522, Japan
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87.Univ South Wales, Pontypridd CF37 1DL, M Glam, Wales
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89.Univ Grenoble Alpes, IPAG, CNRS, F-38000 Grenoble, France
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Recommended Citation
GB/T 7714
Kwon, Woojin,Pattle, Kate,Sadavoy, Sarah,et al. B-fields in Star-forming Region Observations (BISTRO): Magnetic Fields in the Filamentary Structures of Serpens Main[J]. ASTROPHYSICAL JOURNAL,2022,926(2):13.
APA Kwon, Woojin.,Pattle, Kate.,Sadavoy, Sarah.,Hull, Charles L. H..,Johnstone, Doug.,...&van Loo, Sven.(2022).B-fields in Star-forming Region Observations (BISTRO): Magnetic Fields in the Filamentary Structures of Serpens Main.ASTROPHYSICAL JOURNAL,926(2),13.
MLA Kwon, Woojin,et al."B-fields in Star-forming Region Observations (BISTRO): Magnetic Fields in the Filamentary Structures of Serpens Main".ASTROPHYSICAL JOURNAL 926.2(2022):13.
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