Magnetic Fields in Massive Star-forming Regions (MagMaR) IV: Tracing the Magnetic Fields in the O-type protostellar system IRAS 16547$-$4247
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| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| author | Zapata, Luis A. Fernández-López, Manuel Sanhueza, Patricio Girart, Josep M. Rodríguez, Luis F. Cortes, Paulo Patrick, Koch Beltrán, María T. Pattle, Kate Beuther, Henrik Saha, Piyali Jiao, Wenyu Xu, Fengwei Lu, Xing Walker Olguin, Fernando Li, Shanghuo Stephens, Ian W. Kang, Ji-hyun Cheng, Yu Choudhury, Spandan Morii, Kaho Chung, Eun Jung Wang, Jia-Wei Hwang, Jihye Lyo, A-Ran Zhang, Qizhou Chen, Huei-Ru Vivien |
| author_facet | Zapata, Luis A. Fernández-López, Manuel Sanhueza, Patricio Girart, Josep M. Rodríguez, Luis F. Cortes, Paulo Patrick, Koch Beltrán, María T. Pattle, Kate Beuther, Henrik Saha, Piyali Jiao, Wenyu Xu, Fengwei Lu, Xing Walker Olguin, Fernando Li, Shanghuo Stephens, Ian W. Kang, Ji-hyun Cheng, Yu Choudhury, Spandan Morii, Kaho Chung, Eun Jung Wang, Jia-Wei Hwang, Jihye Lyo, A-Ran Zhang, Qizhou Chen, Huei-Ru Vivien |
| contents | The formation of the massive stars, and in particular, the role that the magnetic fields play in their early evolutionary phase is still far from being completely understood. Here, we present Atacama Large Millimeter/Submillimeter Array (ALMA) 1.2 mm full polarized continuum, and H$^{13}$CO$^+$(3$-$2), CS(5$-$4), and HN$^{13}$C(3$-$2) line observations with a high angular resolution ($\sim$0.4$''$ 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 $\sim$10,000 au. This envelope has a bi-conical structure likely carved by the powerful thermal radio jet present in region. The magnetic fields vectors follow very-well the bi-conical envelope. The polarization fraction is $\sim$2.0\% in this region. Some of these vectors seem to converge to IRAS 16547-E, and IRAS 16547-W, the most massive protostars. Moreover, the velocity fields revealed from the spectral lines H$^{13}$CO$^+$(3$-$2), and HN$^{13}$C(3$-$2) show velocity gradients with a good correspondence with the magnetic fields, that maybe are tracing the cavities of molecular outflows or maybe in some parts infall. We derived a magnetic field strength in some filamentary regions that goes from 2 to 6.1\,mG. We also find that the CS(5$-$4) molecular line emission reveals multiple outflow cavities or bow-shocks with different orientations, some of which seem to follow the NW-SE radio thermal jet. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2408_10199 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Magnetic Fields in Massive Star-forming Regions (MagMaR) IV: Tracing the Magnetic Fields in the O-type protostellar system IRAS 16547$-$4247 Zapata, Luis A. Fernández-López, Manuel Sanhueza, Patricio Girart, Josep M. Rodríguez, Luis F. Cortes, Paulo Patrick, Koch Beltrán, María T. Pattle, Kate Beuther, Henrik Saha, Piyali Jiao, Wenyu Xu, Fengwei Lu, Xing Walker Olguin, Fernando Li, Shanghuo Stephens, Ian W. Kang, Ji-hyun Cheng, Yu Choudhury, Spandan Morii, Kaho Chung, Eun Jung Wang, Jia-Wei Hwang, Jihye Lyo, A-Ran Zhang, Qizhou Chen, Huei-Ru Vivien Solar and Stellar Astrophysics Astrophysics of Galaxies The formation of the massive stars, and in particular, the role that the magnetic fields play in their early evolutionary phase is still far from being completely understood. Here, we present Atacama Large Millimeter/Submillimeter Array (ALMA) 1.2 mm full polarized continuum, and H$^{13}$CO$^+$(3$-$2), CS(5$-$4), and HN$^{13}$C(3$-$2) line observations with a high angular resolution ($\sim$0.4$''$ 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 $\sim$10,000 au. This envelope has a bi-conical structure likely carved by the powerful thermal radio jet present in region. The magnetic fields vectors follow very-well the bi-conical envelope. The polarization fraction is $\sim$2.0\% in this region. Some of these vectors seem to converge to IRAS 16547-E, and IRAS 16547-W, the most massive protostars. Moreover, the velocity fields revealed from the spectral lines H$^{13}$CO$^+$(3$-$2), and HN$^{13}$C(3$-$2) show velocity gradients with a good correspondence with the magnetic fields, that maybe are tracing the cavities of molecular outflows or maybe in some parts infall. We derived a magnetic field strength in some filamentary regions that goes from 2 to 6.1\,mG. We also find that the CS(5$-$4) molecular line emission reveals multiple outflow cavities or bow-shocks with different orientations, some of which seem to follow the NW-SE radio thermal jet. |
| title | Magnetic Fields in Massive Star-forming Regions (MagMaR) IV: Tracing the Magnetic Fields in the O-type protostellar system IRAS 16547$-$4247 |
| topic | Solar and Stellar Astrophysics Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2408.10199 |