The Magnetic Field in Quiescent Star-forming Filament G16.96+0.27
We present 850 μ m thermal dust polarization observations with a resolution of 14.″4 (∼0.13 pc) toward an infrared dark cloud G16.96+0.27 using James Clerk Maxwell Telescope/POL-2. The average magnetic field orientation, which roughly agrees with the larger-scale magnetic field orientation traced by...
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad8912 |
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| author | Qi-Lao Gu Tie Liu Zhi-Qiang Shen Sihan Jiao Julien Montillaud Mika Juvela Xing Lu Chang Won Lee Junhao Liu Pak Shing Li Xunchuan Liu Doug Johnstone Woojin Kwon Kee-Tae Kim Ken’ichi Tatematsu Patricio Sanhueza Isabelle Ristorcelli Patrick Koch Qizhou Zhang Kate Pattle Naomi Hirano Dana Alina James Di Francesco |
| author_facet | Qi-Lao Gu Tie Liu Zhi-Qiang Shen Sihan Jiao Julien Montillaud Mika Juvela Xing Lu Chang Won Lee Junhao Liu Pak Shing Li Xunchuan Liu Doug Johnstone Woojin Kwon Kee-Tae Kim Ken’ichi Tatematsu Patricio Sanhueza Isabelle Ristorcelli Patrick Koch Qizhou Zhang Kate Pattle Naomi Hirano Dana Alina James Di Francesco |
| author_sort | Qi-Lao Gu |
| collection | DOAJ |
| description | We present 850 μ m thermal dust polarization observations with a resolution of 14.″4 (∼0.13 pc) toward an infrared dark cloud G16.96+0.27 using James Clerk Maxwell Telescope/POL-2. The average magnetic field orientation, which roughly agrees with the larger-scale magnetic field orientation traced by the Planck 353 GHz data, is approximately perpendicular to the filament structure. The estimated plane-of-sky magnetic field strength is ∼96 μ G and ∼60 μ G using two variants of the Davis–Chandrasekhar–Fermi methods. We calculate the virial and magnetic critical parameters to evaluate the relative importance of gravity, the magnetic field, and turbulence. The magnetic field and turbulence are both weaker than gravity, but magnetic fields and turbulence together are equal to gravity, suggesting that G16.96+0.27 is in a quasi-equilibrium state. The alignment between the magnetic field and cloud is found to have a trend moving away from perpendicularity in the dense regions, which may serve as a tracer of potential fragmentation in such quiescent filaments. |
| format | Article |
| id | doaj-art-bd0b41549256468a8a391f28c1332c46 |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-bd0b41549256468a8a391f28c1332c462024-11-27T05:13:07ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01976224910.3847/1538-4357/ad8912The Magnetic Field in Quiescent Star-forming Filament G16.96+0.27Qi-Lao Gu0https://orcid.org/0000-0002-2826-1902Tie Liu1https://orcid.org/0000-0002-5286-2564Zhi-Qiang Shen2https://orcid.org/0000-0003-3540-8746Sihan Jiao3Julien Montillaud4https://orcid.org/0000-0001-7032-632XMika Juvela5https://orcid.org/0000-0002-5809-4834Xing Lu6https://orcid.org/0000-0003-2619-9305Chang Won Lee7https://orcid.org/0000-0002-3179-6334Junhao Liu8https://orcid.org/0000-0002-4774-2998Pak Shing Li9https://orcid.org/0000-0001-8077-7095Xunchuan Liu10https://orcid.org/0000-0001-8315-4248Doug Johnstone11https://orcid.org/0000-0002-6773-459XWoojin Kwon12https://orcid.org/0000-0003-4022-4132Kee-Tae Kim13https://orcid.org/0000-0003-2412-7092Ken’ichi Tatematsu14https://orcid.org/0000-0002-8149-8546Patricio Sanhueza15https://orcid.org/0000-0002-7125-7685Isabelle Ristorcelli16Patrick Koch17https://orcid.org/0000-0003-2777-5861Qizhou Zhang18https://orcid.org/0000-0003-2384-6589Kate Pattle19https://orcid.org/0000-0002-8557-3582Naomi Hirano20https://orcid.org/0000-0001-9304-7884Dana Alina21https://orcid.org/0000-0001-5403-356XJames Di Francesco22https://orcid.org/0000-0002-9289-2450Shanghai Astronomical Observatory, Chinese Academy of Sciences , No.80 Nandan Road, Xuhui, Shanghai 200030, People's Republic of China ; qlgu@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnShanghai Astronomical Observatory, Chinese Academy of Sciences , No.80 Nandan Road, Xuhui, Shanghai 200030, People's Republic of China ; qlgu@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnShanghai Astronomical Observatory, Chinese Academy of Sciences , No.80 Nandan Road, Xuhui, Shanghai 200030, People's Republic of China ; qlgu@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang, Beijing 100101, People's Republic of ChinaUniversité de Franche-Comté , CNRS, Institut UTINAM, OSU THETA, F-25000 Besançon, FranceDepartment of Physics , PO Box 64, FI-00014, University of Helsinki, FinlandShanghai Astronomical Observatory, Chinese Academy of Sciences , No.80 Nandan Road, Xuhui, Shanghai 200030, People's Republic of China ; qlgu@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnKorea Astronomy and Space Science Institute , 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of Korea; University of Science and Technology , Korea, 217 Gajeong-ro, Yuseong-gu, Daejeon 34113, Republic of KoreaNational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, JapanShanghai Astronomical Observatory, Chinese Academy of Sciences , No.80 Nandan Road, Xuhui, Shanghai 200030, People's Republic of China ; qlgu@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnShanghai Astronomical Observatory, Chinese Academy of Sciences , No.80 Nandan Road, Xuhui, Shanghai 200030, People's Republic of China ; qlgu@shao.ac.cn, liutie@shao.ac.cn, zshen@shao.ac.cnNRC Herzberg Astronomy and Astrophysics , 5071 West Saanich Road, Victoria, BC, V9E 2E7, Canada; Department of Physics and Astronomy, University of Victoria , Victoria, BC, V8P 5C2, CanadaDepartment of Earth Science Education, Seoul National University , 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Republic of Korea; SNU Astronomy Research Center, Seoul National University , 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Republic of Korea; The Center for Educational Research, Seoul National University , 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Republic of KoreaKorea Astronomy and Space Science Institute , 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of Korea; University of Science and Technology , Korea, 217 Gajeong-ro, Yuseong-gu, Daejeon 34113, Republic of KoreaNobeyama Radio Observatory, National Astronomical Observatory of Japan, National Institutes of Natural Sciences Nobeyama , Minamimaki, Minamisaku, Nagano 384-1305, Japan; Astronomical Science Program, Graduate Institute for Advanced Studies , SOKENDAI 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanNational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan; Astronomical Science Program, Graduate Institute for Advanced Studies , SOKENDAI 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanIRAP, Université de Toulouse , CNRS, 9 Avenue du Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, FranceAcademia Sinica Institute of Astronomy and Astrophysics , No. 1, Section 4, Roosevelt Road, Taipei 10617, Taiwan (R.O.C.)Center for Astrophysics ∣ Harvard & Smithsonian , 60 Garden Street, Cambridge, MA 02138, USADepartment of Physics and Astronomy, University College London , Gower Street, London WC1E 6BT, UKAcademia Sinica Institute of Astronomy and Astrophysics , No. 1, Section 4, Roosevelt Road, Taipei 10617, Taiwan (R.O.C.)Department of Physics, School of Science and Technology, Nazarbayev University , Astana 010000, Kazakhstan; IRAP, Université de Toulouse CNRS , UPS, CNES, F-31400 Toulouse, FranceDepartment of Physics and Astronomy, University of Victoria , Victoria, BC, V8W 2Y2, Canada; 2 NRC Herzberg Astronomy and Astrophysics , 5071 West Saanich Road, Victoria, BC, V9E 2E7, CanadaWe present 850 μ m thermal dust polarization observations with a resolution of 14.″4 (∼0.13 pc) toward an infrared dark cloud G16.96+0.27 using James Clerk Maxwell Telescope/POL-2. The average magnetic field orientation, which roughly agrees with the larger-scale magnetic field orientation traced by the Planck 353 GHz data, is approximately perpendicular to the filament structure. The estimated plane-of-sky magnetic field strength is ∼96 μ G and ∼60 μ G using two variants of the Davis–Chandrasekhar–Fermi methods. We calculate the virial and magnetic critical parameters to evaluate the relative importance of gravity, the magnetic field, and turbulence. The magnetic field and turbulence are both weaker than gravity, but magnetic fields and turbulence together are equal to gravity, suggesting that G16.96+0.27 is in a quasi-equilibrium state. The alignment between the magnetic field and cloud is found to have a trend moving away from perpendicularity in the dense regions, which may serve as a tracer of potential fragmentation in such quiescent filaments.https://doi.org/10.3847/1538-4357/ad8912Magnetic fieldsStar formationMolecular cloudsInfrared dark cloudsInterstellar filaments |
| spellingShingle | Qi-Lao Gu Tie Liu Zhi-Qiang Shen Sihan Jiao Julien Montillaud Mika Juvela Xing Lu Chang Won Lee Junhao Liu Pak Shing Li Xunchuan Liu Doug Johnstone Woojin Kwon Kee-Tae Kim Ken’ichi Tatematsu Patricio Sanhueza Isabelle Ristorcelli Patrick Koch Qizhou Zhang Kate Pattle Naomi Hirano Dana Alina James Di Francesco The Magnetic Field in Quiescent Star-forming Filament G16.96+0.27 The Astrophysical Journal Magnetic fields Star formation Molecular clouds Infrared dark clouds Interstellar filaments |
| title | The Magnetic Field in Quiescent Star-forming Filament G16.96+0.27 |
| title_full | The Magnetic Field in Quiescent Star-forming Filament G16.96+0.27 |
| title_fullStr | The Magnetic Field in Quiescent Star-forming Filament G16.96+0.27 |
| title_full_unstemmed | The Magnetic Field in Quiescent Star-forming Filament G16.96+0.27 |
| title_short | The Magnetic Field in Quiescent Star-forming Filament G16.96+0.27 |
| title_sort | magnetic field in quiescent star forming filament g16 96 0 27 |
| topic | Magnetic fields Star formation Molecular clouds Infrared dark clouds Interstellar filaments |
| url | https://doi.org/10.3847/1538-4357/ad8912 |
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