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| Dust polarized emission observations of NGC 6334 BISTRO reveals the details of the complex but organized magnetic field structure of the high-mass star-forming hub-filament network | |
Arzoumanian, D.1,2; Furuya, R. S.3; Hasegawa, T.4; Tahani, M.5; Sadavoy, S.6; Hull, C. L. H.7,8; Johnstone, D.9,10; Koch, P. M.11; Inutsuka, S.2; Doi, Y.12; Hoang, T.13,14; Onaka, T.15,16; Iwasaki, K.4; Shimajiri, Y.4; Inoue, T.2; Peretto, N.17; Andre, P.18; Bastien, P.19,20; Berry, D.21; Chen, H. -R. V.11,22,23; Di Francesco, J.9,10; Eswaraiah, C.24,25; Fanciullo, L.11; Fissel, L. M.6; Hwang, J.13,14; Kang, J. -h.13; Kim, G.26; Kim, K. -T.13,14; Kirchschlager, F.27; Kwon, W.28; Lee, C. W.13,14; Liu, H. -L.29,30; Lyo, A. -R.13; Pattle, K.31; Soam, A.32; Tang, X.33 ; Whitworth, A.17; Ching, T. -C.24,25; Coude, S.32; Wang, J. -W.11; Ward-Thompson, D.34; Lai, S. -P.11,22,23; Qiu, K.35,36; Bourke, T. L.37,38; Byun, D. -Y.13,14; Chen, M.10; Chen, Z.39; Chen, W. P.40; Cho, J.41; Choi, Y.13; Choi, M.13; Chrysostomou, A.37,42; Chung, E. J.41; Dai, S.25; Diep, P. N.43; Duan, H. -Y.22,23; Duan, Y.25; Eden, D.44; Fiege, J.45; Franzmann, E.45; Friberg, P.21; Fuller, G.46; Gledhill, T.42; Graves, S.21; Greaves, J.17; Griffin, M.17; Gu, Q.47; Han, I.13,14; Hatchell, J.48; Hayashi, S.49; Houde, M.50; Jeong, I. -G.13; Kang, M.13; Kang, S. -j.13; Kataoka, A.4; Kawabata, K.51,52,53; Kemper, F.11,54; Kim, M. -R.13; Kim, K. H.13; Kim, J.13,14; Kim, S.13,14; Kirk, J.34; Kobayashi, M. I. N.55; Konyves, V.34; Kusune, T.4; Kwon, J.16; Lacaille, K.56,57; Law, C. -Y.47,58; Lee, C. -F.11; Lee, Y. -H.21,59; Lee, S. -S.13,14; Lee, H.41; Lee, J. -E.59; Li, H. -b.47; Li, D.60,61; Li, D. L.33; Liu, J.62,63; Liu, T.64; Liu, S. -Y.11; Lu, X.4; Mairs, S.21; Matsumura, M.65,66; Matthews, B.9,10; Moriarty-Schieven, G.9; Nagata, T.67; Nakamura, F.4,68; Nakanishi, H.69; Ngoc, N. B.43; Ohashi, N.49; Park, G.13; Parsons, H.21; Pyo, T. -S.49,68; Qian, L.24; Rao, R.11; Rawlings, J.27; Rawlings, M.21; Retter, B.17; Richer, J.70,71; Rigby, A.17; Saito, H.72; Savini, G.27; Scaife, A.46; Seta, M.73; Shinnaga, H.69; Tamura, M.4,16,74; Tang, Y. -W.11; Tomisaka, K.4,68; Tram, L. N.75; Tsukamoto, Y.69; Viti, S.27; Wang, H.39; Xie, J.25; Yen, H. -W.11; Yoo, H.13; Yuan, J.25; Yun, H. -S.59; Zenko, T.67; Zhang, G.24; Zhang, C. -P.24,25; Zhang, Y.47; Zhou, J.33; Zhu, L.24; de Looze, I.27; Dowell, C. D.76; Eyres, S.77; Falle, S.78; Friesen, R.79; Robitaille, J. -F.80; van Loo, S.81
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| 2021-03-11 | |
| Source Publication | ASTRONOMY & ASTROPHYSICS
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| ISSN | 0004-6361 |
| Volume | 647Pages:A78 |
| Contribution Rank | 31 |
| Abstract | Context. Molecular filaments and hubs have received special attention recently thanks to new studies showing their key role in star formation. While the (column) density and velocity structures of both filaments and hubs have been carefully studied, their magnetic field (B-field) properties have yet to be characterized. Consequently, the role of B-fields in the formation and evolution of hub-filament systems is not well constrained. Aims. We aim to understand the role of the B-field and its interplay with turbulence and gravity in the dynamical evolution of the NGC 6334 filament network that harbours cluster-forming hubs and high-mass star formation. Methods. We present new observations of the dust polarized emission at 850 mu m toward the 2 pc x 10 pc map of NGC 6334 at a spatial resolution of 0.09 pc obtained with the James Clerk Maxwell Telescope (JCMT) as part of the B-field In STar-forming Region Observations (BISTRO) survey. We study the distribution and dispersion of the polarized intensity (PI), the polarization fraction (PF), and the plane-of-the-sky B-field angle (chi(BPOS)) toward the whole region, along the 10 pc-long ridge and along the sub-filaments connected to the ridge and the hubs. We derived the power spectra of the intensity and chi(BPOS) along the ridge crest and compared them with the results obtained from simulated filaments. Results. The observations span similar to 3 orders of magnitude in Stokes I and PI and similar to 2 orders of magnitude in PF (from similar to 0.2 to similar to 20%). A large scatter in PI and PF is observed for a given value of I. Our analyses show a complex B-field structure when observed over the whole region (similar to 10 pc); however, at smaller scales (similar to 1 chi(BPOS) varies coherently along the crests of the filament network. The observed power spectrum of chi(BPOS) can be well represented with a power law function with a slope of -1.33 +/- 0.23, which is similar to 20% shallower than that of I. We find that this result is compatible with the properties of simulated filaments and may indicate the physical processes at play in the formation and evolution of star-forming filaments. Along the sub-filaments, chi(BPOS) rotates from being mostly perpendicular or randomly oriented with respect to the crests to mostly parallel as the sub-filaments merge with the ridge and hubs. This variation of the B-field structure along the sub-filaments may be tracing local velocity flows of infalling matter in the ridge and hubs. Our analysis also suggests a variation in the energy balance along the crests of these sub-filaments, from magnetically critical or supercritical at their far ends to magnetically subcritical near the ridge and hubs. We also detect an increase in PF toward the high-column density (N-H2 greater than or similar to 10(23) cm(-2)) star cluster-forming hubs. These latter large PF values may be explained by the increase in grain alignment efficiency due to stellar radiation from the newborn stars, combined with an ordered B-field structure. Conclusions. These observational results reveal for the first time the characteristics of the small-scale (down to similar to 0.1 pc) B-field structure of a 10 pc-long hub-filament system. Our analyses show variations in the polarization properties along the sub-filaments that may be tracing the evolution of their physical properties during their interaction with the ridge and hubs. We also detect an impact of feedback from young high-mass stars on the local B-field structure and the polarization properties, which could put constraints on possible models for dust grain alignment and provide important hints as to the interplay between the star formation activity and interstellar B-fields. |
| Keyword | stars: formation submillimeter: ISM ISM: magnetic fields ISM: structure polarization ISM: clouds |
| DOI | 10.1051/0004-6361/202038624 |
| URL | 查看原文 |
| Indexed By | SCI |
| Language | 英语 |
| Funding Project | FCT/MCTES through national funds (PIDDAC)[UID/FIS/04434/2019] ; FCT/MCTES through national funds (PIDDAC)[UIDB/04434/2020] ; Japan Society for Promotion of Science[KAKENHI 19H0193810] ; NAOJ Fellowship ; JSPS KAKENHI[18K13586] ; JSPS KAKENHI[20K14527] ; JSPS KAKENHI[18H01250] ; JSPS KAKENHI[18H05442] ; JSPS KAKENHI[15H02063] ; JSPS KAKENHI[22000005] ; JSPS KAKENHI[19K14775] ; National Research Council of Canada ; Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery Grants ; Ministry of Science and Technology (MOST) in Taiwan[MOST 108-2112-M-001-012] ; Ministry of Science and Technology (MOST) in Taiwan[MOST 109-2112-M-001-022] ; Academia Sinica Career Development Award ; National Key R&D Program of China[2017YFA0402600] ; National Key R&D Program of China[2017YFA0402700] ; National Natural Science Foundation of China (NSFC)[U1731237] ; National Research Foundation of Korea (NRF) - Ministry of Education, Science and Technology[2019R1A2C1010851] ; Seoul National University ; National Research Foundation of Korea[NRF-2016R1C1B2013642] ; JCMT BISTRO Large Program[M17BL011] ; Science and Technology Facilities Council of the United Kingdom ; Canada Foundation for Innovation |
| WOS Research Area | Astronomy & Astrophysics |
| WOS Subject | Astronomy & Astrophysics |
| WOS ID | WOS:000629649400001 |
| Publisher | EDP SCIENCES S A |
| Funding Organization | FCT/MCTES through national funds (PIDDAC) ; Japan Society for Promotion of Science ; NAOJ Fellowship ; JSPS KAKENHI ; National Research Council of Canada ; Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery Grants ; Ministry of Science and Technology (MOST) in Taiwan ; Academia Sinica Career Development Award ; National Key R&D Program of China ; National Natural Science Foundation of China (NSFC) ; National Research Foundation of Korea (NRF) - Ministry of Education, Science and Technology ; Seoul National University ; National Research Foundation of Korea ; JCMT BISTRO Large Program ; Science and Technology Facilities Council of the United Kingdom ; Canada Foundation for Innovation |
| Citation statistics | |
| Document Type | 期刊论文 |
| Identifier | http://ir.xao.ac.cn/handle/45760611-7/3981 |
| Collection | 射电天文研究室_恒星形成与演化研究团组 |
| Corresponding Author | Arzoumanian, D. |
| Affiliation | 1.Univ Porto, Inst Astrofis & Ciencias Espaco, CAUP, Rua Estrelas, P-4150762 Porto, Portugal 2.Nagoya Univ, Grad Sch Sci, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648602, Japan 3.Tokushima Univ, Inst Liberal Arts & Sci, Minami Jousanajima Machi 1-1, Tokushima 7708502, Japan 4.Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan 5.Natl Res Council Canada, Herzberg Astron & Astrophys Res Ctr, Domin Radio Astrophys Observ, POB 248, Penticton, BC V2A 6J9, Canada 6.Queens Univ, Dept Phys Engn Phys & Astrophys, Kingston, ON K7L 3N6, Canada 7.NAOJ Chile, Natl Astron Observ Japan, Alonso Cordova 3788,Off 61B, Santiago 7630422, Chile 8.Joint ALMA Observ, Alonso Cordova 3107, Santiago, Chile 9.NRC Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada 10.Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 2Y2, Canada 11.Acad Sinica, Inst Astron & Astrophys, 1,Sec 4,Roosevelt Rd, Taipei 10617, Taiwan 12.Univ Tokyo, Grad Sch Arts & Sci, Dept Earth Sci & 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Inst Astron, Madingley Rd, Cambridge CB3 0HA, England 72.Univ Tsukuba, Fac Pure & Appl Sci, 1-1-1 Tennodai, Tsukuba, Ibaraki 3058577, Japan 73.Kwansei Gakuin Univ, Sch Sci & Technol, Dept Phys, 2-1 Gakuen, Sanda, Hyogo 6691337, Japan 74.Natl Inst Nat Sci, Astrobiol Ctr, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan 75.Univ Sci & Technol Hanoi, Vietnam Acad Sci & Technol, 18 Hoang Quoc Viet, Hanoi, Vietnam 76.Jet Prop Lab, M-S 169-506,4800 Oak Grove Dr, Pasadena, CA 91109 USA 77.Univ South Wales, Pontypridd CF37 1DL, M Glam, Wales 78.Univ Leeds, Dept Appl Math, Wood House Lane, Leeds LS2 9JT, W Yorkshire, England 79.Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA 80.Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France 81.Univ Leeds, Sch Phys & Astron, Woodhouse Lane, Leeds LS2 9JT, W Yorkshire, England |
| Recommended Citation GB/T 7714 | Arzoumanian, D.,Furuya, R. S.,Hasegawa, T.,et al. Dust polarized emission observations of NGC 6334 BISTRO reveals the details of the complex but organized magnetic field structure of the high-mass star-forming hub-filament network[J]. ASTRONOMY & ASTROPHYSICS,2021,647:A78. |
| APA | Arzoumanian, D..,Furuya, R. S..,Hasegawa, T..,Tahani, M..,Sadavoy, S..,...&van Loo, S..(2021).Dust polarized emission observations of NGC 6334 BISTRO reveals the details of the complex but organized magnetic field structure of the high-mass star-forming hub-filament network.ASTRONOMY & ASTROPHYSICS,647,A78. |
| MLA | Arzoumanian, D.,et al."Dust polarized emission observations of NGC 6334 BISTRO reveals the details of the complex but organized magnetic field structure of the high-mass star-forming hub-filament network".ASTRONOMY & ASTROPHYSICS 647(2021):A78. |
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