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

Abstract 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 ( B POS ) toward the high-mass star-forming region G333.46−0.16 (G333), obtained with the Atacama Large Millimeter/submillimeter Array at 1.2 mm as part of the Magnetic fields in Massive star-forming Regions survey. The B POS morphology found in this region is consistent with a canonical “hourglass” with an embedded flattened envelope in a perpendicular direction, which suggests a dynamically important field. This region is fragmented into two protostars that appear to be gravitationally bound in a stable binary system with a separation of ∼1740 au. Interestingly, by analyzing H 13 CO + ( J = 3–2) line emission, we find no velocity gradient over the extent of the continuum, which is consistent with a strong field. We model the B POS , obtaining a marginally supercritical mass-to-flux ratio of 1.43, suggesting an initially strongly magnetized environment. Based on the Davis–Chandrasekhar–Fermi method, the magnetic field strength toward G333 is estimated to be 5.7 mG. The absence of strong rotation and outflows toward 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.

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Publication Details

Journal
The Astrophysical Journal Letters
Published
2024-08-22
DOI
https://doi.org/10.3847/2041-8213/ad660c
Citations
12
Primary Topic
Astrophysics and Star Formation Studies
Type
article
Field-Weighted Citation Impact
3.98

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article

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

Paulo C. Cortés, Eun Jung Chung, Piyali Saha, Jihye Hwang et al.
12 citations
The Astrophysical Journal Letters
Astrophysics and Star Formation Studies
3.98
article

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

Paulo C. Cortés, Eun Jung Chung, Piyali Saha, Jihye Hwang, Patricio Sanhueza, Luis A. Zapata, Shanghuo Li, Fengwei Xu, Ji‐hyun Kang, Yu Cheng, Patrick M. Koch, Huei-Ru Vivien Chen, Janik Karoly, Spandan Choudhury, Kaho Morii, Á. Sánchez-Monge, Wenyu Jiao, Xing Lu, M. Padovani, Kate Pattle, J. M. Girart, Chi-Yan Law, Fernando A. Olguin, M. T. Beltrán, Ian Stephens, T. Csengeri, H. Beuther, Charles L. H. Hull, Shantanu Basu, Daniele Galli, Manuel Fernández-López, Fumitaka Nakamura, Jia-Wei Wang, Jongsoo Kim, Qizhou Zhang, Junhao Liu
article en
12 citations

Abstract

Abstract 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 ( B POS ) toward the high-mass star-forming region G333.46−0.16 (G333), obtained with the Atacama Large Millimeter/submillimeter Array at 1.2 mm as part of the Magnetic fields in Massive star-forming Regions survey. The B POS morphology found in this region is consistent with a canonical “hourglass” with an embedded flattened envelope in a perpendicular direction, which suggests a dynamically important field. This region is fragmented into two protostars that appear to be gravitationally bound in a stable binary system with a separation of ∼1740 au. Interestingly, by analyzing H 13 CO + ( J = 3–2) line emission, we find no velocity gradient over the extent of the continuum, which is consistent with a strong field. We model the B POS , obtaining a marginally supercritical mass-to-flux ratio of 1.43, suggesting an initially strongly magnetized environment. Based on the Davis–Chandrasekhar–Fermi method, the magnetic field strength toward G333 is estimated to be 5.7 mG. The absence of strong rotation and outflows toward 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.

The Astrophysical Journal LettersVol. 972(1)
Western University (CA), Centre National de la Recherche Scientifique (FR), Institute of Astronomy and Astrophysics, Academia Sinica (TW), Institute of Space Sciences (ES), Université de Bordeaux (FR), Consejo Nacional de Investigaciones Científicas y Técnicas (AR), University of Cologne (DE), National Institutes of Natural Sciences (JP), The Graduate University for Advanced Studies, SOKENDAI (JP), Peking University (CN), National Tsing Hua University (TW), National Radio Astronomy Observatory (US), Atacama Large Millimeter Submillimeter Array (CL), Shanghai Astronomical Observatory (CN), Arcetri Astrophysical Observatory (IT), Korea Astronomy and Space Science Institute (KR), Worcester State University (US), Institut d'Estudis Espacials de Catalunya (ES), Laboratoire d'Astrophysique de Bordeaux (FR), Kavli Institute for Theoretical Sciences (CN), Max Planck Institute for Astronomy (DE), Center for Astrophysics Harvard & Smithsonian (US), Instituto Argentino de Radioastronomía (AR), National Astronomical Observatory of Japan (JP), University College London (GB), The University of Tokyo (JP), Universidad Nacional Autónoma de México (MX)
National Science Foundation, Natural Science Foundation of Shanghai, National Radio Astronomy Observatory, European Commission, National Natural Science Foundation of China, Chinese Academy of Sciences, Korea Astronomy and Space Science Institute, National Astronomical Observatory of Japan, Science and Technology Facilities Council, Research Executive Agency, Japan Society for the Promotion of Science, National Institutes of Natural Sciences, Agencia Estatal de Investigación
Openalex Percentile: Top 6%
Astrophysics and Star Formation Studies
3.98
DOIOpen Access PDFOpenAlex
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