MagMaR III—Resisting the Pressure, Is the Magnetic Field Overwhelmed in NGC6334I?
- Autores
- Cortés, Paulo C.; Girart, Josep M.; Sanhueza, Patricio; Liu, Junhao; Martín, Sergio; Stephens, Ian; Beuther, Henrik; Koch, Patrick M.; Fernandez Lopez, Manuel; Sánchez Monge, Álvaro; Wang, Jia Wei; Morii, Kaho; Li, Shanghuo; Saha, Piyali; Zhang, Qizhou; Rebolledo, David; Zapata Gonzalez, Luis Alberto; Kang, Ji hyun; Jiao, Wenyu; Kim, Jongsoo; Cheng, Yu; Hwang, Jihye; Chung, Eun Jung; Choudhury, Spandan; Lyo, A. Ran; Olguin, Fernando
- Año de publicación
- 2024
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We report on Atacama Large Millimeter/submillimeter Array observations of polarized dust emission at 1.2 mm from NGC6334I, a source known for its significant flux outbursts. Between five months, our data show no substantial change in total intensity and a modest 8% variation in linear polarization, suggesting a phase of stability or the conclusion of the outburst. The magnetic field, inferred from this polarized emission, displays a predominantly radial pattern from northwest to southeast with intricate disturbances across major cores, hinting at spiral structures. Energy analysis of CS (J = 5 → 4) emission yields an outflow energy of approximately 3.5 × 1045 erg, aligning with previous interferometric studies. Utilizing the Davis–Chandrasekhar–Fermi method, we determined magnetic field strengths ranging from 1 to 11 mG, averaging at 1.9 mG. This average increases to 4 ± 1 mG when incorporating Zeeman measurements. Comparative analyses using gravitational, thermal, and kinetic energy maps reveal that magnetic energy is significantly weaker, possibly explaining the observed field morphology. We also find that the energy in the outflows and the expanding cometary HII region is also larger than the magnetic energy, suggesting that protostellar feedback may be the dominant driver behind the injection of turbulence in NGC6334I at the scales sampled by our data. The gas in NGC6334I predominantly exhibits supersonic and trans-Alfvenic conditions, transitioning towards a super-Alfvenic regime, underscoring a diminished influence of the magnetic field with increasing gas density. These observations are in agreement with prior polarization studies at 220 GHz, enriching our understanding of the dynamic processes in high-mass star-forming regions.
Fil: Cortés, Paulo C.. Joint ALMA Observatory; Chile
Fil: Girart, Josep M.. Institut de Ciéncies de l’Espai; España
Fil: Sanhueza, Patricio. National Astronomical Observatory of Japan; Japón
Fil: Liu, Junhao. National Astronomical Observatory of Japan; Japón
Fil: Martín, Sergio. Joint ALMA Observatory; Chile
Fil: Stephens, Ian. Worcester State University; Estados Unidos
Fil: Beuther, Henrik. Max Planck Institute for Radio Astronomy; Alemania
Fil: Koch, Patrick M.. Academia Sinica; China
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: Sánchez Monge, Álvaro. Institut de Ciéncies de l’Espai; España
Fil: Wang, Jia Wei. Academia Sinica; China
Fil: Morii, Kaho. The University of Tokyo; Japón
Fil: Li, Shanghuo. Max Planck Institute for Radio Astronomy; Japón
Fil: Saha, Piyali. National Astronomical Observatory of Japan; Japón
Fil: Zhang, Qizhou. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
Fil: Rebolledo, David. Joint ALMA Observatory; Chile
Fil: Zapata Gonzalez, Luis Alberto. Universidad Nacional Autónoma de México; México
Fil: Kang, Ji hyun. Korea Astronomy And Space Science Institute; Corea del Sur
Fil: Jiao, Wenyu. Peking University; China
Fil: Kim, Jongsoo. Korea Astronomy And Space Science Institute; Corea del Sur
Fil: Cheng, Yu. National Astronomical Observatory of Japan; Japón
Fil: Hwang, Jihye. Korea Astronomy And Space Science Institute; Corea del Sur
Fil: Chung, Eun Jung. Korea Astronomy And Space Science Institute; Corea del Sur
Fil: Choudhury, Spandan. Korea Astronomy And Space Science Institute; Corea del Sur
Fil: Lyo, A. Ran. Korea Astronomy And Space Science Institute; Corea del Sur
Fil: Olguin, Fernando. National Tsing Hua University; China - Materia
-
Interstellar magnetic fields
Star Formation - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/268521
Ver los metadatos del registro completo
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MagMaR III—Resisting the Pressure, Is the Magnetic Field Overwhelmed in NGC6334I?Cortés, Paulo C.Girart, Josep M.Sanhueza, PatricioLiu, JunhaoMartín, SergioStephens, IanBeuther, HenrikKoch, Patrick M.Fernandez Lopez, ManuelSánchez Monge, ÁlvaroWang, Jia WeiMorii, KahoLi, ShanghuoSaha, PiyaliZhang, QizhouRebolledo, DavidZapata Gonzalez, Luis AlbertoKang, Ji hyunJiao, WenyuKim, JongsooCheng, YuHwang, JihyeChung, Eun JungChoudhury, SpandanLyo, A. RanOlguin, FernandoInterstellar magnetic fieldsStar Formationhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We report on Atacama Large Millimeter/submillimeter Array observations of polarized dust emission at 1.2 mm from NGC6334I, a source known for its significant flux outbursts. Between five months, our data show no substantial change in total intensity and a modest 8% variation in linear polarization, suggesting a phase of stability or the conclusion of the outburst. The magnetic field, inferred from this polarized emission, displays a predominantly radial pattern from northwest to southeast with intricate disturbances across major cores, hinting at spiral structures. Energy analysis of CS (J = 5 → 4) emission yields an outflow energy of approximately 3.5 × 1045 erg, aligning with previous interferometric studies. Utilizing the Davis–Chandrasekhar–Fermi method, we determined magnetic field strengths ranging from 1 to 11 mG, averaging at 1.9 mG. This average increases to 4 ± 1 mG when incorporating Zeeman measurements. Comparative analyses using gravitational, thermal, and kinetic energy maps reveal that magnetic energy is significantly weaker, possibly explaining the observed field morphology. We also find that the energy in the outflows and the expanding cometary HII region is also larger than the magnetic energy, suggesting that protostellar feedback may be the dominant driver behind the injection of turbulence in NGC6334I at the scales sampled by our data. The gas in NGC6334I predominantly exhibits supersonic and trans-Alfvenic conditions, transitioning towards a super-Alfvenic regime, underscoring a diminished influence of the magnetic field with increasing gas density. These observations are in agreement with prior polarization studies at 220 GHz, enriching our understanding of the dynamic processes in high-mass star-forming regions.Fil: Cortés, Paulo C.. Joint ALMA Observatory; ChileFil: Girart, Josep M.. Institut de Ciéncies de l’Espai; EspañaFil: Sanhueza, Patricio. National Astronomical Observatory of Japan; JapónFil: Liu, Junhao. National Astronomical Observatory of Japan; JapónFil: Martín, Sergio. Joint ALMA Observatory; ChileFil: Stephens, Ian. Worcester State University; Estados UnidosFil: Beuther, Henrik. Max Planck Institute for Radio Astronomy; AlemaniaFil: Koch, Patrick M.. Academia Sinica; ChinaFil: 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: Sánchez Monge, Álvaro. Institut de Ciéncies de l’Espai; EspañaFil: Wang, Jia Wei. Academia Sinica; ChinaFil: Morii, Kaho. The University of Tokyo; JapónFil: Li, Shanghuo. Max Planck Institute for Radio Astronomy; JapónFil: Saha, Piyali. National Astronomical Observatory of Japan; JapónFil: Zhang, Qizhou. Harvard-Smithsonian Center for Astrophysics; Estados UnidosFil: Rebolledo, David. Joint ALMA Observatory; ChileFil: Zapata Gonzalez, Luis Alberto. Universidad Nacional Autónoma de México; MéxicoFil: Kang, Ji hyun. Korea Astronomy And Space Science Institute; Corea del SurFil: Jiao, Wenyu. Peking University; ChinaFil: Kim, Jongsoo. Korea Astronomy And Space Science Institute; Corea del SurFil: Cheng, Yu. National Astronomical Observatory of Japan; JapónFil: Hwang, Jihye. Korea Astronomy And Space Science Institute; Corea del SurFil: Chung, Eun Jung. Korea Astronomy And Space Science Institute; Corea del SurFil: Choudhury, Spandan. Korea Astronomy And Space Science Institute; Corea del SurFil: Lyo, A. Ran. Korea Astronomy And Space Science Institute; Corea del SurFil: Olguin, Fernando. National Tsing Hua University; ChinaIOP Publishing2024-08info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/268521Cortés, Paulo C.; Girart, Josep M.; Sanhueza, Patricio; Liu, Junhao; Martín, Sergio; et al.; MagMaR III—Resisting the Pressure, Is the Magnetic Field Overwhelmed in NGC6334I?; IOP Publishing; Astrophysical Journal; 972; 1; 8-2024; 1-270004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ad59a7info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ad59a7info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T12:18:31Zoai:ri.conicet.gov.ar:11336/268521instacron: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:34982025-10-22 12:18:31.259CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
MagMaR III—Resisting the Pressure, Is the Magnetic Field Overwhelmed in NGC6334I? |
| title |
MagMaR III—Resisting the Pressure, Is the Magnetic Field Overwhelmed in NGC6334I? |
| spellingShingle |
MagMaR III—Resisting the Pressure, Is the Magnetic Field Overwhelmed in NGC6334I? Cortés, Paulo C. Interstellar magnetic fields Star Formation |
| title_short |
MagMaR III—Resisting the Pressure, Is the Magnetic Field Overwhelmed in NGC6334I? |
| title_full |
MagMaR III—Resisting the Pressure, Is the Magnetic Field Overwhelmed in NGC6334I? |
| title_fullStr |
MagMaR III—Resisting the Pressure, Is the Magnetic Field Overwhelmed in NGC6334I? |
| title_full_unstemmed |
MagMaR III—Resisting the Pressure, Is the Magnetic Field Overwhelmed in NGC6334I? |
| title_sort |
MagMaR III—Resisting the Pressure, Is the Magnetic Field Overwhelmed in NGC6334I? |
| dc.creator.none.fl_str_mv |
Cortés, Paulo C. Girart, Josep M. Sanhueza, Patricio Liu, Junhao Martín, Sergio Stephens, Ian Beuther, Henrik Koch, Patrick M. Fernandez Lopez, Manuel Sánchez Monge, Álvaro Wang, Jia Wei Morii, Kaho Li, Shanghuo Saha, Piyali Zhang, Qizhou Rebolledo, David Zapata Gonzalez, Luis Alberto Kang, Ji hyun Jiao, Wenyu Kim, Jongsoo Cheng, Yu Hwang, Jihye Chung, Eun Jung Choudhury, Spandan Lyo, A. Ran Olguin, Fernando |
| author |
Cortés, Paulo C. |
| author_facet |
Cortés, Paulo C. Girart, Josep M. Sanhueza, Patricio Liu, Junhao Martín, Sergio Stephens, Ian Beuther, Henrik Koch, Patrick M. Fernandez Lopez, Manuel Sánchez Monge, Álvaro Wang, Jia Wei Morii, Kaho Li, Shanghuo Saha, Piyali Zhang, Qizhou Rebolledo, David Zapata Gonzalez, Luis Alberto Kang, Ji hyun Jiao, Wenyu Kim, Jongsoo Cheng, Yu Hwang, Jihye Chung, Eun Jung Choudhury, Spandan Lyo, A. Ran Olguin, Fernando |
| author_role |
author |
| author2 |
Girart, Josep M. Sanhueza, Patricio Liu, Junhao Martín, Sergio Stephens, Ian Beuther, Henrik Koch, Patrick M. Fernandez Lopez, Manuel Sánchez Monge, Álvaro Wang, Jia Wei Morii, Kaho Li, Shanghuo Saha, Piyali Zhang, Qizhou Rebolledo, David Zapata Gonzalez, Luis Alberto Kang, Ji hyun Jiao, Wenyu Kim, Jongsoo Cheng, Yu Hwang, Jihye Chung, Eun Jung Choudhury, Spandan Lyo, A. Ran Olguin, Fernando |
| 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 |
| dc.subject.none.fl_str_mv |
Interstellar magnetic fields Star Formation |
| topic |
Interstellar magnetic fields Star Formation |
| purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
| dc.description.none.fl_txt_mv |
We report on Atacama Large Millimeter/submillimeter Array observations of polarized dust emission at 1.2 mm from NGC6334I, a source known for its significant flux outbursts. Between five months, our data show no substantial change in total intensity and a modest 8% variation in linear polarization, suggesting a phase of stability or the conclusion of the outburst. The magnetic field, inferred from this polarized emission, displays a predominantly radial pattern from northwest to southeast with intricate disturbances across major cores, hinting at spiral structures. Energy analysis of CS (J = 5 → 4) emission yields an outflow energy of approximately 3.5 × 1045 erg, aligning with previous interferometric studies. Utilizing the Davis–Chandrasekhar–Fermi method, we determined magnetic field strengths ranging from 1 to 11 mG, averaging at 1.9 mG. This average increases to 4 ± 1 mG when incorporating Zeeman measurements. Comparative analyses using gravitational, thermal, and kinetic energy maps reveal that magnetic energy is significantly weaker, possibly explaining the observed field morphology. We also find that the energy in the outflows and the expanding cometary HII region is also larger than the magnetic energy, suggesting that protostellar feedback may be the dominant driver behind the injection of turbulence in NGC6334I at the scales sampled by our data. The gas in NGC6334I predominantly exhibits supersonic and trans-Alfvenic conditions, transitioning towards a super-Alfvenic regime, underscoring a diminished influence of the magnetic field with increasing gas density. These observations are in agreement with prior polarization studies at 220 GHz, enriching our understanding of the dynamic processes in high-mass star-forming regions. Fil: Cortés, Paulo C.. Joint ALMA Observatory; Chile Fil: Girart, Josep M.. Institut de Ciéncies de l’Espai; España Fil: Sanhueza, Patricio. National Astronomical Observatory of Japan; Japón Fil: Liu, Junhao. National Astronomical Observatory of Japan; Japón Fil: Martín, Sergio. Joint ALMA Observatory; Chile Fil: Stephens, Ian. Worcester State University; Estados Unidos Fil: Beuther, Henrik. Max Planck Institute for Radio Astronomy; Alemania Fil: Koch, Patrick M.. Academia Sinica; China 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: Sánchez Monge, Álvaro. Institut de Ciéncies de l’Espai; España Fil: Wang, Jia Wei. Academia Sinica; China Fil: Morii, Kaho. The University of Tokyo; Japón Fil: Li, Shanghuo. Max Planck Institute for Radio Astronomy; Japón Fil: Saha, Piyali. National Astronomical Observatory of Japan; Japón Fil: Zhang, Qizhou. Harvard-Smithsonian Center for Astrophysics; Estados Unidos Fil: Rebolledo, David. Joint ALMA Observatory; Chile Fil: Zapata Gonzalez, Luis Alberto. Universidad Nacional Autónoma de México; México Fil: Kang, Ji hyun. Korea Astronomy And Space Science Institute; Corea del Sur Fil: Jiao, Wenyu. Peking University; China Fil: Kim, Jongsoo. Korea Astronomy And Space Science Institute; Corea del Sur Fil: Cheng, Yu. National Astronomical Observatory of Japan; Japón Fil: Hwang, Jihye. Korea Astronomy And Space Science Institute; Corea del Sur Fil: Chung, Eun Jung. Korea Astronomy And Space Science Institute; Corea del Sur Fil: Choudhury, Spandan. Korea Astronomy And Space Science Institute; Corea del Sur Fil: Lyo, A. Ran. Korea Astronomy And Space Science Institute; Corea del Sur Fil: Olguin, Fernando. National Tsing Hua University; China |
| description |
We report on Atacama Large Millimeter/submillimeter Array observations of polarized dust emission at 1.2 mm from NGC6334I, a source known for its significant flux outbursts. Between five months, our data show no substantial change in total intensity and a modest 8% variation in linear polarization, suggesting a phase of stability or the conclusion of the outburst. The magnetic field, inferred from this polarized emission, displays a predominantly radial pattern from northwest to southeast with intricate disturbances across major cores, hinting at spiral structures. Energy analysis of CS (J = 5 → 4) emission yields an outflow energy of approximately 3.5 × 1045 erg, aligning with previous interferometric studies. Utilizing the Davis–Chandrasekhar–Fermi method, we determined magnetic field strengths ranging from 1 to 11 mG, averaging at 1.9 mG. This average increases to 4 ± 1 mG when incorporating Zeeman measurements. Comparative analyses using gravitational, thermal, and kinetic energy maps reveal that magnetic energy is significantly weaker, possibly explaining the observed field morphology. We also find that the energy in the outflows and the expanding cometary HII region is also larger than the magnetic energy, suggesting that protostellar feedback may be the dominant driver behind the injection of turbulence in NGC6334I at the scales sampled by our data. The gas in NGC6334I predominantly exhibits supersonic and trans-Alfvenic conditions, transitioning towards a super-Alfvenic regime, underscoring a diminished influence of the magnetic field with increasing gas density. These observations are in agreement with prior polarization studies at 220 GHz, enriching our understanding of the dynamic processes in high-mass star-forming regions. |
| publishDate |
2024 |
| dc.date.none.fl_str_mv |
2024-08 |
| 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/11336/268521 Cortés, Paulo C.; Girart, Josep M.; Sanhueza, Patricio; Liu, Junhao; Martín, Sergio; et al.; MagMaR III—Resisting the Pressure, Is the Magnetic Field Overwhelmed in NGC6334I?; IOP Publishing; Astrophysical Journal; 972; 1; 8-2024; 1-27 0004-637X CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/268521 |
| identifier_str_mv |
Cortés, Paulo C.; Girart, Josep M.; Sanhueza, Patricio; Liu, Junhao; Martín, Sergio; et al.; MagMaR III—Resisting the Pressure, Is the Magnetic Field Overwhelmed in NGC6334I?; IOP Publishing; Astrophysical Journal; 972; 1; 8-2024; 1-27 0004-637X CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
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eng |
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info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ad59a7 info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ad59a7 |
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info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
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openAccess |
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https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
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application/pdf application/pdf |
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IOP Publishing |
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IOP Publishing |
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dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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