Magnetic Fields in Massive Star-forming Regions (MagMaR): Unveiling an Hourglass Magnetic Field in G333.46-0.16 using ALMA
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2024
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| author | Saha, Piyali Sanhueza, Patricio Padovani, Marco Girart, Josep M. Cortes, Paulo Morii, Kaho Liu, Junhao Sanchez-Monge, A. Galli, Daniele Basu, Shantanu Koch, Patrick M. Beltran, Maria T. Li, Shanghuo Beuther, Henrik Stephens, Ian W. Nakamura, Fumitaka Zhang, Qizhou Jiao, Wenyu Fernandez-Lopez, 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. |
| author_facet | Saha, Piyali Sanhueza, Patricio Padovani, Marco Girart, Josep M. Cortes, Paulo Morii, Kaho Liu, Junhao Sanchez-Monge, A. Galli, Daniele Basu, Shantanu Koch, Patrick M. Beltran, Maria T. Li, Shanghuo Beuther, Henrik Stephens, Ian W. Nakamura, Fumitaka Zhang, Qizhou Jiao, Wenyu Fernandez-Lopez, 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. |
| contents | The contribution of the magnetic field to the formation of high-mass stars is poorly understood. We report the high-angular resolution ($\sim0.3^{\prime\prime}$, 870 au) map of the magnetic field projected on the plane of the sky (B$_\mathrm{POS}$) towards the high-mass star forming region G333.46$-$0.16 (G333), obtained with the Atacama Large Millimeter/submillimeter Array (ALMA) at 1.2 mm as part of the Magnetic Fields in Massive Star-forming Regions (MagMaR) survey. The B$_\mathrm{POS}$ 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 $\sim1740$ au. Interestingly, by analysing H$^{13}$CO$^{+}$ ($J=3-2$) line emission, we find no velocity gradient over the extend of the continuum which is consistent with a strong field. We model the B$_\mathrm{POS}$, 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 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. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2407_16654 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Magnetic Fields in Massive Star-forming Regions (MagMaR): Unveiling an Hourglass Magnetic Field in G333.46-0.16 using ALMA Saha, Piyali Sanhueza, Patricio Padovani, Marco Girart, Josep M. Cortes, Paulo Morii, Kaho Liu, Junhao Sanchez-Monge, A. Galli, Daniele Basu, Shantanu Koch, Patrick M. Beltran, Maria T. Li, Shanghuo Beuther, Henrik Stephens, Ian W. Nakamura, Fumitaka Zhang, Qizhou Jiao, Wenyu Fernandez-Lopez, 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. Astrophysics of Galaxies The contribution of the magnetic field to the formation of high-mass stars is poorly understood. We report the high-angular resolution ($\sim0.3^{\prime\prime}$, 870 au) map of the magnetic field projected on the plane of the sky (B$_\mathrm{POS}$) towards the high-mass star forming region G333.46$-$0.16 (G333), obtained with the Atacama Large Millimeter/submillimeter Array (ALMA) at 1.2 mm as part of the Magnetic Fields in Massive Star-forming Regions (MagMaR) survey. The B$_\mathrm{POS}$ 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 $\sim1740$ au. Interestingly, by analysing H$^{13}$CO$^{+}$ ($J=3-2$) line emission, we find no velocity gradient over the extend of the continuum which is consistent with a strong field. We model the B$_\mathrm{POS}$, 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 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. |
| title | Magnetic Fields in Massive Star-forming Regions (MagMaR): Unveiling an Hourglass Magnetic Field in G333.46-0.16 using ALMA |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2407.16654 |