Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247
- Autores
- Zapata, Luis A.; Fernandez Lopez, Manuel; Sanhueza, Patricio; Girart, Josep M.; Rodríguez, Luis Fernando; Cortés, Paulo; Koch, Patrick; Beltrán, Maria T.; Pattle, Kate; Beuther, Henrik; Saha, Piyali; Jiao, Wenyu; Xu, Fengwei; Lu, Xing Walker; Olguin, Fernando; Li, Shanghuo; Stephens, Ian; Kang, Ji hyun; Cheng, Yu; Choudhury, Spandan; Morii, Kaho; Chung, Eun Jung; Wang, Jia Wei; Hwang, Jihye; Lyo, A Ran; Zhang, Q.; Chen, Huei Ru Vivien
- Año de publicación
- 2024
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- 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 H13CO+(3‑2), CS(5‑4), and HN13C(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 H13CO+(3‑2) and HN13C(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.
Fil: Zapata, Luis A.. Universidad Nacional Autónoma de México; México
Fil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Sanhueza, Patricio. Consejo Superior de Investigaciones Cientificas. Instituto Nacional de Tecnica Aeroespacial. Departamento de Cargas Utiles y Ciencias del Espacio; España. National Astronomical Observatory Of Japan; Japón
Fil: Girart, Josep M.. Institut d’Estudis Espacials de Catalunya; España
Fil: Rodríguez, Luis Fernando. Universidad Nacional Autónoma de México; México
Fil: Cortés, Paulo. Joint Alma Observatory; Chile. National Radio Astronomy Observatory; Estados Unidos
Fil: Koch, Patrick. Istituto Nazionale di Astrofisica; Italia
Fil: Beltrán, Maria T.. Istituto Nazionale di Astrofisica; Italia
Fil: Pattle, Kate. University College London; Estados Unidos
Fil: Beuther, Henrik. Max Planck Institute For Radio Astronomy; Alemania
Fil: Saha, Piyali. National Institutes of Natural Sciences; Japón
Fil: Jiao, Wenyu. Peking University; China
Fil: Xu, Fengwei. Peking University; China
Fil: Lu, Xing Walker. Chinese Academy of Sciences; República de China
Fil: Olguin, Fernando. National Tsing Hua University; China
Fil: Li, Shanghuo. Max Planck Institute For Radio Astronomy; Alemania
Fil: Stephens, Ian. Worcester State University; Estados Unidos
Fil: Kang, Ji hyun. Korea Astronomy and Space Science Institute; Corea del Sur
Fil: Cheng, Yu. National Astronomical Observatory of Japan; Japón
Fil: Choudhury, Spandan. Korea Astronomy And Space Science Institute; Corea del Sur
Fil: Morii, Kaho. National Astronomical Observatory of Japan; Argentina
Fil: Chung, Eun Jung. Korea Astronomy And Space Science Institute; Corea del Sur
Fil: Wang, Jia Wei. National Tsing Hua University; China
Fil: Hwang, Jihye. Korea Astronomy And Space Science Institute; Corea del Sur
Fil: Lyo, A Ran. Korea Astronomy And Space Science Institute; Corea del Sur
Fil: Zhang, Q.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Chen, Huei Ru Vivien. National Tsing Hua University; China - Materia
-
Star formation
Astrophysics - Solar and Stellar Astrophysics
Astrophysics - Astrophysics of Galaxies - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/267341
Ver los metadatos del registro completo
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Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247Zapata, Luis A.Fernandez Lopez, ManuelSanhueza, PatricioGirart, Josep M.Rodríguez, Luis FernandoCortés, PauloKoch, PatrickBeltrán, Maria T.Pattle, KateBeuther, HenrikSaha, PiyaliJiao, WenyuXu, FengweiLu, Xing WalkerOlguin, FernandoLi, ShanghuoStephens, IanKang, Ji hyunCheng, YuChoudhury, SpandanMorii, KahoChung, Eun JungWang, Jia WeiHwang, JihyeLyo, A RanZhang, Q.Chen, Huei Ru VivienStar formationAstrophysics - Solar and Stellar AstrophysicsAstrophysics - Astrophysics of Galaxieshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The 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 H13CO+(3‑2), CS(5‑4), and HN13C(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 H13CO+(3‑2) and HN13C(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.Fil: Zapata, Luis A.. Universidad Nacional Autónoma de México; MéxicoFil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaFil: Sanhueza, Patricio. Consejo Superior de Investigaciones Cientificas. Instituto Nacional de Tecnica Aeroespacial. Departamento de Cargas Utiles y Ciencias del Espacio; España. National Astronomical Observatory Of Japan; JapónFil: Girart, Josep M.. Institut d’Estudis Espacials de Catalunya; EspañaFil: Rodríguez, Luis Fernando. Universidad Nacional Autónoma de México; MéxicoFil: Cortés, Paulo. Joint Alma Observatory; Chile. National Radio Astronomy Observatory; Estados UnidosFil: Koch, Patrick. Istituto Nazionale di Astrofisica; ItaliaFil: Beltrán, Maria T.. Istituto Nazionale di Astrofisica; ItaliaFil: Pattle, Kate. University College London; Estados UnidosFil: Beuther, Henrik. Max Planck Institute For Radio Astronomy; AlemaniaFil: Saha, Piyali. National Institutes of Natural Sciences; JapónFil: Jiao, Wenyu. Peking University; ChinaFil: Xu, Fengwei. Peking University; ChinaFil: Lu, Xing Walker. Chinese Academy of Sciences; República de ChinaFil: Olguin, Fernando. National Tsing Hua University; ChinaFil: Li, Shanghuo. Max Planck Institute For Radio Astronomy; AlemaniaFil: Stephens, Ian. Worcester State University; Estados UnidosFil: Kang, Ji hyun. Korea Astronomy and Space Science Institute; Corea del SurFil: Cheng, Yu. National Astronomical Observatory of Japan; JapónFil: Choudhury, Spandan. Korea Astronomy And Space Science Institute; Corea del SurFil: Morii, Kaho. National Astronomical Observatory of Japan; ArgentinaFil: Chung, Eun Jung. Korea Astronomy And Space Science Institute; Corea del SurFil: Wang, Jia Wei. National Tsing Hua University; ChinaFil: Hwang, Jihye. Korea Astronomy And Space Science Institute; Corea del SurFil: Lyo, A Ran. Korea Astronomy And Space Science Institute; Corea del SurFil: Zhang, Q.. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Chen, Huei Ru Vivien. National Tsing Hua University; ChinaIOP Publishing2024-10info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/267341Zapata, Luis A.; Fernandez Lopez, Manuel; Sanhueza, Patricio; Girart, Josep M.; Rodríguez, Luis Fernando; et al.; Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247; IOP Publishing; Astrophysical Journal; 974; 2; 10-2024; 1-100004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ad701dinfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ad701dinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:36:08Zoai:ri.conicet.gov.ar:11336/267341instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 09:36:08.772CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247 |
| title |
Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247 |
| 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. Star formation Astrophysics - Solar and Stellar Astrophysics Astrophysics - Astrophysics of Galaxies |
| title_short |
Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247 |
| title_full |
Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247 |
| title_fullStr |
Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247 |
| title_full_unstemmed |
Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247 |
| title_sort |
Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247 |
| dc.creator.none.fl_str_mv |
Zapata, Luis A. Fernandez Lopez, Manuel Sanhueza, Patricio Girart, Josep M. Rodríguez, Luis Fernando Cortés, Paulo Koch, Patrick Beltrán, Maria T. Pattle, Kate Beuther, Henrik Saha, Piyali Jiao, Wenyu Xu, Fengwei Lu, Xing Walker Olguin, Fernando Li, Shanghuo Stephens, Ian Kang, Ji hyun Cheng, Yu Choudhury, Spandan Morii, Kaho Chung, Eun Jung Wang, Jia Wei Hwang, Jihye Lyo, A Ran Zhang, Q. Chen, Huei Ru Vivien |
| author |
Zapata, Luis A. |
| author_facet |
Zapata, Luis A. Fernandez Lopez, Manuel Sanhueza, Patricio Girart, Josep M. Rodríguez, Luis Fernando Cortés, Paulo Koch, Patrick Beltrán, Maria T. Pattle, Kate Beuther, Henrik Saha, Piyali Jiao, Wenyu Xu, Fengwei Lu, Xing Walker Olguin, Fernando Li, Shanghuo Stephens, Ian Kang, Ji hyun Cheng, Yu Choudhury, Spandan Morii, Kaho Chung, Eun Jung Wang, Jia Wei Hwang, Jihye Lyo, A Ran Zhang, Q. Chen, Huei Ru Vivien |
| author_role |
author |
| author2 |
Fernandez Lopez, Manuel Sanhueza, Patricio Girart, Josep M. Rodríguez, Luis Fernando Cortés, Paulo Koch, Patrick Beltrán, Maria T. Pattle, Kate Beuther, Henrik Saha, Piyali Jiao, Wenyu Xu, Fengwei Lu, Xing Walker Olguin, Fernando Li, Shanghuo Stephens, Ian Kang, Ji hyun Cheng, Yu Choudhury, Spandan Morii, Kaho Chung, Eun Jung Wang, Jia Wei Hwang, Jihye Lyo, A Ran Zhang, Q. Chen, Huei Ru Vivien |
| author2_role |
author author author author author author author author author author author author author author author author author author author author author author author author author author |
| dc.subject.none.fl_str_mv |
Star formation Astrophysics - Solar and Stellar Astrophysics Astrophysics - Astrophysics of Galaxies |
| topic |
Star formation Astrophysics - Solar and Stellar Astrophysics Astrophysics - Astrophysics of Galaxies |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
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 H13CO+(3‑2), CS(5‑4), and HN13C(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 H13CO+(3‑2) and HN13C(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. Fil: Zapata, Luis A.. Universidad Nacional Autónoma de México; México Fil: Fernandez Lopez, Manuel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina Fil: Sanhueza, Patricio. Consejo Superior de Investigaciones Cientificas. Instituto Nacional de Tecnica Aeroespacial. Departamento de Cargas Utiles y Ciencias del Espacio; España. National Astronomical Observatory Of Japan; Japón Fil: Girart, Josep M.. Institut d’Estudis Espacials de Catalunya; España Fil: Rodríguez, Luis Fernando. Universidad Nacional Autónoma de México; México Fil: Cortés, Paulo. Joint Alma Observatory; Chile. National Radio Astronomy Observatory; Estados Unidos Fil: Koch, Patrick. Istituto Nazionale di Astrofisica; Italia Fil: Beltrán, Maria T.. Istituto Nazionale di Astrofisica; Italia Fil: Pattle, Kate. University College London; Estados Unidos Fil: Beuther, Henrik. Max Planck Institute For Radio Astronomy; Alemania Fil: Saha, Piyali. National Institutes of Natural Sciences; Japón Fil: Jiao, Wenyu. Peking University; China Fil: Xu, Fengwei. Peking University; China Fil: Lu, Xing Walker. Chinese Academy of Sciences; República de China Fil: Olguin, Fernando. National Tsing Hua University; China Fil: Li, Shanghuo. Max Planck Institute For Radio Astronomy; Alemania Fil: Stephens, Ian. Worcester State University; Estados Unidos Fil: Kang, Ji hyun. Korea Astronomy and Space Science Institute; Corea del Sur Fil: Cheng, Yu. National Astronomical Observatory of Japan; Japón Fil: Choudhury, Spandan. Korea Astronomy And Space Science Institute; Corea del Sur Fil: Morii, Kaho. National Astronomical Observatory of Japan; Argentina Fil: Chung, Eun Jung. Korea Astronomy And Space Science Institute; Corea del Sur Fil: Wang, Jia Wei. National Tsing Hua University; China Fil: Hwang, Jihye. Korea Astronomy And Space Science Institute; Corea del Sur Fil: Lyo, A Ran. Korea Astronomy And Space Science Institute; Corea del Sur Fil: Zhang, Q.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Chen, Huei Ru Vivien. National Tsing Hua University; China |
| description |
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 H13CO+(3‑2), CS(5‑4), and HN13C(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 H13CO+(3‑2) and HN13C(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. |
| publishDate |
2024 |
| dc.date.none.fl_str_mv |
2024-10 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
| format |
article |
| status_str |
publishedVersion |
| dc.identifier.none.fl_str_mv |
http://hdl.handle.net/11336/267341 Zapata, Luis A.; Fernandez Lopez, Manuel; Sanhueza, Patricio; Girart, Josep M.; Rodríguez, Luis Fernando; et al.; Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247; IOP Publishing; Astrophysical Journal; 974; 2; 10-2024; 1-10 0004-637X CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/267341 |
| identifier_str_mv |
Zapata, Luis A.; Fernandez Lopez, Manuel; Sanhueza, Patricio; Girart, Josep M.; Rodríguez, Luis Fernando; et al.; Magnetic Fields in Massive Star-forming Regions (MagMaR). IV. Tracing the Magnetic Fields in the O-type Protostellar System IRAS 16547–4247; IOP Publishing; Astrophysical Journal; 974; 2; 10-2024; 1-10 0004-637X CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
| language |
eng |
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info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by/2.5/ar/ |
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openAccess |
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application/pdf application/pdf |
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IOP Publishing |
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IOP Publishing |
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