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
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/268521

id CONICETDig_97e66e78b72e806375f47c3b814d4df6
oai_identifier_str oai:ri.conicet.gov.ar:11336/268521
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling 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 Técnicas2025-09-29T10:45:12Zoai: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:34982025-09-29 10:45:13.2CONICET 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
language eng
dc.relation.none.fl_str_mv 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
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv IOP Publishing
publisher.none.fl_str_mv IOP Publishing
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
_version_ 1844614491324547072
score 13.070432