The Astrophysical Journal (Jan 2024)
Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247
- Luis A. Zapata,
- Manuel Fernández-López,
- Patricio Sanhueza,
- Josep M. Girart,
- Luis F. Rodríguez,
- Paulo Cortés,
- Patrick Koch,
- Maria T. Beltrán,
- Kate Pattle,
- Henrik Beuther,
- Piyali Saha,
- Wenyu Jiao,
- Fengwei Xu,
- Xing Walker Lu,
- Fernando Olguin,
- Shanghuo Li,
- Ian W. Stephens,
- Ji-hyun Kang,
- Yu Cheng,
- Spandan Choudhury,
- Kaho Morii,
- Eun Jung Chung,
- Jia-Wei Wang,
- Jihye Hwang,
- A-Ran Lyo,
- Q. Zhang,
- Huei-Ru Vivien Chen
Affiliations
- Luis A. Zapata
- ORCiD
- Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México , P.O. Box 3-72, 58090, Morelia, Michoacán, Mexico ; [email protected]
- Manuel Fernández-López
- ORCiD
- Instituto Argentino de Radioastronomía (CCT-La Plata, CONICET; CICPBA) , C.C. No. 5, 1894, Villa Elisa, Buenos Aires, Argentina
- Patricio Sanhueza
- ORCiD
- National Astronomical Observatory of Japan, National Institutes of Natural Sciences , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies) , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
- Josep M. Girart
- ORCiD
- Institut d’Estudis Espacials de Catalunya (IEEC) , c/Gran Capita, 2-4, E-08034 Barcelona, Catalonia, Spain
- Luis F. Rodríguez
- ORCiD
- Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México , P.O. Box 3-72, 58090, Morelia, Michoacán, Mexico ; [email protected]
- Paulo Cortés
- ORCiD
- Joint ALMA Observatory , Alonso de Córdova 3107, Vitacura, Santiago, Chile; National Radio Astronomy Observatory , 520 Edgemont Road, Charlottesville, VA 22903, USA
- Patrick Koch
- ORCiD
- Institute of Astronomy and Astrophysics , Academia Sinica, No. 1, Sec. 4, Roosevelt Road, Taipei 10617, Taiwan
- Maria T. Beltrán
- ORCiD
- INAF-Osservatorio Astrofisico di Arcetri , Largo E. Fermi 5, I-50125 Firenze, Italy
- Kate Pattle
- ORCiD
- Department of Physics and Astronomy, University College London , Gower Street, London WC1E 6BT, UK
- Henrik Beuther
- ORCiD
- Max Planck Institute for Astronomy , Konigstuhl 17, D-69117 Heidelberg, Germany
- Piyali Saha
- ORCiD
- National Astronomical Observatory of Japan, National Institutes of Natural Sciences , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
- Wenyu Jiao
- ORCiD
- Department of Astronomy, School of Physics, Peking University , Beijing 100871, People's Republic of China; Kavli Institute for Astronomy and Astrophysics, Peking University , Haidian District, Beijing 100871, People's Republic of China
- Fengwei Xu
- ORCiD
- Department of Astronomy, School of Physics, Peking University , Beijing 100871, People's Republic of China; I. Physikalisches Institut, Universität zu Köln , Zülpicher Str. 77, D-50937 Köln, Germany; Kavli Institute for Astronomy and Astrophysics, Peking University , Beijing 100871, People's Republic of China
- Xing Walker Lu
- ORCiD
- Shanghai Astronomical Observatory, Chinese Academy of Sciences , 80 Nandan Road, Xuhui, Shanghai 200030, People's Republic of China
- Fernando Olguin
- ORCiD
- Institute of Astronomy and Department of Physics, National Tsing Hua University , Hsinchu 30013, Taiwan
- Shanghuo Li
- ORCiD
- Max Planck Institute for Astronomy , Konigstuhl 17, D-69117 Heidelberg, Germany
- Ian W. Stephens
- ORCiD
- Department of Earth, Environment, and Physics, Worcester State University , Worcester, MA 01602, USA
- Ji-hyun Kang
- ORCiD
- Korea Astronomy and Space Science Institute , 776 Daedeok-daero, Yuseong, Daejeon 34055, Republic of Korea
- Yu Cheng
- ORCiD
- National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
- Spandan Choudhury
- ORCiD
- Korea Astronomy and Space Science Institute , 776 Daedeok-daero Yuseong-gu, Daejeon 34055, Republic of Korea
- Kaho Morii
- ORCiD
- National Astronomical Observatory of Japan, National Institutes of Natural Sciences , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Department of Astronomy, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
- Eun Jung Chung
- ORCiD
- Korea Astronomy and Space Science Institute , 776 Daedeokdae-ro, Yuseong-gu, Daejeon, Republic of Korea
- Jia-Wei Wang
- ORCiD
- Institute of Astronomy and Department of Physics, National Tsing Hua University , Hsinchu 30013, Taiwan
- Jihye Hwang
- ORCiD
- Korea Astronomy and Space Science Institute (KASI) , 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of Korea
- A-Ran Lyo
- ORCiD
- Korea Astronomy and Space Science Institute (KASI) , 776 Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of Korea
- Q. Zhang
- ORCiD
- Center for Astrophysics, Harvard & Smithsonian , 60 Garden Street, Cambridge, MA 02138, USA
- Huei-Ru Vivien Chen
- ORCiD
- Institute of Astronomy and Department of Physics, National Tsing Hua University , Hsinchu 300044, Taiwan
- DOI
- https://doi.org/10.3847/1538-4357/ad701d
- Journal volume & issue
-
Vol. 974,
no. 2
p. 257
Abstract
The formation of the massive stars, and in particular, the role that the magnetic fields play in their early evolutionary phase is still far from being completely understood. Here, we present the Atacama Large Millimeter/submillimeter Array 1.2 mm full polarized continuum and H ^13 CO ^+ (3−2), CS(5−4), and HN ^13 C(3−2) line observations with a high angular resolution (∼0.″4 or 1100 au). In the 1.2 mm continuum emission, we reveal a dusty envelope surrounding the massive protostars, IRAS16547-E and IRAS16547-W, with dimensions of ∼10,000 au. This envelope has a biconical structure likely carved by the powerful thermal radio jet present in region. The magnetic field vectors follow very well the biconical envelope. The polarization fraction is ∼2.0% in this region. Some of these vectors seem to converge to IRAS 16547-E and IRAS 16547-W, the most massive protostars. Moreover, the velocity fields revealed from the spectral lines H ^13 CO ^+ (3−2) and HN ^13 C(3−2) show velocity gradients with a good correspondence with the magnetic fields, which maybe are tracing the cavities of molecular outflows or maybe infalling in some parts. We derived a magnetic field strength in some filamentary regions that goes from 2 to 6.1 mG. We also find that the CS(5−4) molecular line emission reveals multiple outflow cavities or bow shocks with different orientations, some of which seem to follow the NW–SE radio thermal jet.
Keywords
