Magnetic Fields in Massive Star-forming Regions (MagMaR). VI. Magnetic Field Dragging in the Filamentary High-mass Star-forming Region G35.20--0.74N due to Gravity
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2025
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| author | Hwang, Jihye Sanhueza, Patricio Girart, Josep Miquel Stephens, Ian W. Beltrán, Maria T. Law, Chi Yan Zhang, Qizhou Liu, Junhao Cortés, Paulo Olguin, Fernando A. Koch, Patrick M. Nakamura, Fumitaka Saha, Piyali Wang, Jia-Wei Xu, Fengwei Beuther, Henrik Morii, Kaho López, Manuel Fernández Jiao, Wenyu Kim, Kee-Tae Li, Shanghuo Zapata, Luis A. Kim, Jongsoo Choudhury, Spandan Cheng, Yu Pattle, Kate Eswaraiah, Chakali Sandhyarani, Panigrahy Dewangan, L. K. Jadhav, O. R. |
| author_facet | Hwang, Jihye Sanhueza, Patricio Girart, Josep Miquel Stephens, Ian W. Beltrán, Maria T. Law, Chi Yan Zhang, Qizhou Liu, Junhao Cortés, Paulo Olguin, Fernando A. Koch, Patrick M. Nakamura, Fumitaka Saha, Piyali Wang, Jia-Wei Xu, Fengwei Beuther, Henrik Morii, Kaho López, Manuel Fernández Jiao, Wenyu Kim, Kee-Tae Li, Shanghuo Zapata, Luis A. Kim, Jongsoo Choudhury, Spandan Cheng, Yu Pattle, Kate Eswaraiah, Chakali Sandhyarani, Panigrahy Dewangan, L. K. Jadhav, O. R. |
| contents | We investigate the magnetic field orientation and strength in the massive star-forming region G35.20-0.74N (G35), using polarized dust emission data obtained with the Atacama Large Millimeter/submillimeter Array (ALMA) as part of the Magnetic fields in Massive star-forming Regions (MagMaR) survey. The G35 region shows a filamentary structure (a length of $\sim$0.1 pc) with six bright cores located along the filament's long axis. Magnetic field strengths across the G35 region range from 0.2 to 4.4 mG with a mean value of 0.8 $\pm$ 0.4 mG. The mass-to-flux ratio ($λ$) varies from 0.1 to 6.0 the critical value. The highest values are found locally around cores, whereas the remains of the filament are subcritical. A H$^{13}$CO$^+$ (3--2) velocity gradient of 29 km s$^{-1}$ pc$^{-1}$ is evident along the filament's long axis, aligned with the magnetic field direction. At larger scales ($\sim$0.1 pc), the magnetic field lines appear roughly perpendicular to the filament's long axis, in contrast to the smaller-scale structure ($\sim$0.003 pc) traced by ALMA. The magnetic field lines could be dragged along the filament as a result of the gas motion induced by the gravitational potential of the filament. Six cores in the filament have similar spacings between 0.02--0.04 pc. The initial filament fragmentation could have produced a core spacing of 0.06 pc, following filament fragmentation theory, and the current core spacing is the result of cores comoving with the gas along the filament. This core migration could occur in a few 10$^4$ years, consistent with high-mass star formation time scales. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2510_25078 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Magnetic Fields in Massive Star-forming Regions (MagMaR). VI. Magnetic Field Dragging in the Filamentary High-mass Star-forming Region G35.20--0.74N due to Gravity Hwang, Jihye Sanhueza, Patricio Girart, Josep Miquel Stephens, Ian W. Beltrán, Maria T. Law, Chi Yan Zhang, Qizhou Liu, Junhao Cortés, Paulo Olguin, Fernando A. Koch, Patrick M. Nakamura, Fumitaka Saha, Piyali Wang, Jia-Wei Xu, Fengwei Beuther, Henrik Morii, Kaho López, Manuel Fernández Jiao, Wenyu Kim, Kee-Tae Li, Shanghuo Zapata, Luis A. Kim, Jongsoo Choudhury, Spandan Cheng, Yu Pattle, Kate Eswaraiah, Chakali Sandhyarani, Panigrahy Dewangan, L. K. Jadhav, O. R. Astrophysics of Galaxies We investigate the magnetic field orientation and strength in the massive star-forming region G35.20-0.74N (G35), using polarized dust emission data obtained with the Atacama Large Millimeter/submillimeter Array (ALMA) as part of the Magnetic fields in Massive star-forming Regions (MagMaR) survey. The G35 region shows a filamentary structure (a length of $\sim$0.1 pc) with six bright cores located along the filament's long axis. Magnetic field strengths across the G35 region range from 0.2 to 4.4 mG with a mean value of 0.8 $\pm$ 0.4 mG. The mass-to-flux ratio ($λ$) varies from 0.1 to 6.0 the critical value. The highest values are found locally around cores, whereas the remains of the filament are subcritical. A H$^{13}$CO$^+$ (3--2) velocity gradient of 29 km s$^{-1}$ pc$^{-1}$ is evident along the filament's long axis, aligned with the magnetic field direction. At larger scales ($\sim$0.1 pc), the magnetic field lines appear roughly perpendicular to the filament's long axis, in contrast to the smaller-scale structure ($\sim$0.003 pc) traced by ALMA. The magnetic field lines could be dragged along the filament as a result of the gas motion induced by the gravitational potential of the filament. Six cores in the filament have similar spacings between 0.02--0.04 pc. The initial filament fragmentation could have produced a core spacing of 0.06 pc, following filament fragmentation theory, and the current core spacing is the result of cores comoving with the gas along the filament. This core migration could occur in a few 10$^4$ years, consistent with high-mass star formation time scales. |
| title | Magnetic Fields in Massive Star-forming Regions (MagMaR). VI. Magnetic Field Dragging in the Filamentary High-mass Star-forming Region G35.20--0.74N due to Gravity |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2510.25078 |