Magnetic Fields in Massive Star-forming Regions (MagMaR): Unveiling an Hourglass Magnetic Field in G333.46−0.16 using ALMA

作     者：Saha, Piyali Sanhueza, Patricio Padovani, Marco Girart, Josep M. Cortes, Paulo Morii, Kaho Liu, Junhao Sánchez-Monge, Á. Galli, Daniele Basu, Shantanu Koch, Patrick M. Beltrán, Maria T. Li, Shanghuo Beuther, Henrik Stephens, Ian W. Nakamura, Fumitaka Zhang, Qizhou Jiao, Wenyu Fernández-López, M. Hwang, Jihye Chung, Eun Jung Pattle, Kate Zapata, Luis A. Xu, Fengwei Olguin, Fernando A. Kang, Ji-Hyun Karoly, Janik Law, Chi-Yan Wang, Jia-Wei Csengeri, Timea Lu, Xing Cheng, Yu Kim, Jongsoo Choudhury, Spandan Chen, Huei-Ru Vivien Hull, Charles L.H. 

作者机构：National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Astronomical Science Program The Graduate University for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-8588 Japan INAF-Osservatorio Astrofisico di Arcetri Largo E. Fermi 5 Firenze50125 Italy  Campus UAB Can Magrans S/N Cerdanyola del Vallés CataloniaE-08193 Spain  PMT-UPC Esteve Terradas 1 Castelldefels CataloniaE-08860 Spain Joint ALMA Observatory Alonso de Córdova 3107 Vitacura Santiago Chile National Radio Astronomy Observatory 520 Edgemont Road CharlottesvilleVA22903 United States Department of Astronomy Graduate School of Science The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan Department of Physics and Astronomy University of Western Ontario LondonONN6A 3K7 Canada Academia Sinica Institute of Astronomy and Astrophysics Taipei Taiwan INAF-Osservatorio Astrofisico di Arcetri Largo E. Fermi 5 FirenzeI-50125 Italy Max Planck Institute for Astronomy Königstuhl 17 HeidelbergD-69117 Germany Department of Earth Environment and Physics Worcester State University WorcesterMA01602 United States Department of Astronomy The University of Tokyo Hongo Tokyo113-0033 Japan  2-21-1 Osawa Mitaka Tokyo181-0015 Japan Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Department of Astronomy School of Physics Peking University Beijing100871 China Kavli Institute for Astronomy and Astrophysics Peking University Haidian District Beijing100871 China  C.C. No. 5 Villa Elisa Buenos Aires1894 Argentina Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejeon34055 Korea Republic of Department of Physics and Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Instituto de Radioastronomía y Astrofísica Universidad Nacional Autónoma de México P.O. Box 3-72 Michoacán Morelia58090 Mexico I. Physikalisches Institut Universität zu Köln Zülpicher Str. 77 KölnD-50937 Germany Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Institute of Astronomy National Tsing Hua University Hsinchu30013 Taiwan Department of Physics and Astronomy University College London LondonWC1E 6BT United Kingdom Institute of Astronomy Department of Physics National Tsing Hua University Hsinchu30013 Taiwan Laboratoire d’astrophysique de Bordeaux Univ. Bordeaux CNRS B18N allée Geoffroy Saint-Hilaire Pessac33615 France Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Institute of Astronomy Department of Physics National Tsing Hua University Hsinchu300044 Taiwan 

出 版 物：《arXiv》 (arXiv)

年 卷 期：2024年

核心收录：

主　　题：Magnetic fields 

摘      要：The contribution of the magnetic field to the formation of high-mass stars is poorly understood. We report the high-angular resolution (∼ 0.3′′, 870 au) map of the magnetic field projected on the plane of the sky (Bpos) towards the high-mass star forming region G333.46−0.16 (G333), obtained with the Atacama Large Millimeter/submillimeter Array (ALMA) at 1.2 mm as part of the Magnetic Fields in Massive Star-forming Regions (MagMaR) survey. The Bpos morphology found in this region is consistent with a canonical hourglass which suggest a dynamically important field. This region is fragmented into two protostars separated by ∼ 1740 au. Interestingly, by analysing H13CO+ (J = 3−2) line emission, we find no velocity gradient over the extend of the continuum which is consistent with a strong field. We model the Bpos, obtaining a marginally supercritical mass-to-flux ratio of 1.43, suggesting a initially strongly magnetized environment. Based on the Davis–Chandrasekhar–Fermi method, the magnetic field strength towards G333 is estimated to be 5.7 mG. The absence of strong rotation and outflows towards the central region of G333 suggests strong magnetic braking, consistent with a highly magnetized environment. Our study shows that despite being a strong regulator, the magnetic energy fails to prevent the process of fragmentation, as revealed by the formation of the two protostars in the central region. Copyright © 2024, The Authors. All rights reserved.