Magnetic Fields in the Pillars of Creation

Autores
Sarkar, Adwitiya; Looney, Leslie W.; Pound, Marc W.; Li, Zhi Yun; Stephens, Ian W.; Fernandez Lopez, Manuel; Coudé, Simon; Lin, Zhe-Yu Daniel; Yang, Haifeng; Faistl, Reid
Año de publicación
2025
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Due to dust grain alignment with magnetic fields, dust polarization observations of far-infrared emission from cold molecular clouds are often used to trace magnetic fields, allowing a probe of the effects of magnetic fields on the star formation process. We present inferred magnetic field maps of the Pillars of Creation region within the larger M16 emission nebula, derived from dust polarization data in the 89 and 154 μm continuum using the Stratospheric Observatory For Infrared Astronomy/High-resolution Airborne Wideband Camera. We derive magnetic field strength estimates using the Davis–Chandrasekhar–Fermi method. We compare the polarization and magnetic field strengths to column densities and dust continuum intensities across the region to build a coherent picture of the relationship between star-forming activity and magnetic fields in the region. The projected magnetic field strengths derived are in the range of ∼50–130 μG, which is typical for clouds of similar n(H2), i.e., molecular hydrogen volume density on the order of 104–105 cm‑3. We conclude that star formation occurs in the finger tips when the magnetic fields are too weak to prevent radial collapse due to gravity but strong enough to oppose OB stellar radiation pressure, while in the base of the fingers the magnetic fields hinder mass accretion and consequently star formation. We also support an initial weak-field model (<50 μG) with subsequent strengthening through realignment and compression, resulting in a dynamically important magnetic field.
Fil: Sarkar, Adwitiya. University of Illinois at Urbana; Estados Unidos
Fil: Looney, Leslie W.. University of Illinois at Urbana; Estados Unidos
Fil: Pound, Marc W.. University of Maryland; Estados Unidos
Fil: Li, Zhi Yun. University of Virginia; Estados Unidos
Fil: Stephens, Ian W.. Worcester Polytechnic Institute; Estados Unidos
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: Coudé, Simon. Worcester Polytechnic Institute; Estados Unidos
Fil: Lin, Zhe-Yu Daniel. University of Virginia; Estados Unidos
Fil: Yang, Haifeng. Zhejiang University; China
Fil: Faistl, Reid. University of Illinois at Urbana; Estados Unidos
Materia
Polarimetry
Dust continuum emission
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:11336/278971
Acceder
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network_name_str CONICET Digital (CONICET)
spelling Magnetic Fields in the Pillars of CreationSarkar, AdwitiyaLooney, Leslie W.Pound, Marc W.Li, Zhi YunStephens, Ian W.Fernandez Lopez, ManuelCoudé, SimonLin, Zhe-Yu DanielYang, HaifengFaistl, ReidPolarimetryDust continuum emissionhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Due to dust grain alignment with magnetic fields, dust polarization observations of far-infrared emission from cold molecular clouds are often used to trace magnetic fields, allowing a probe of the effects of magnetic fields on the star formation process. We present inferred magnetic field maps of the Pillars of Creation region within the larger M16 emission nebula, derived from dust polarization data in the 89 and 154 μm continuum using the Stratospheric Observatory For Infrared Astronomy/High-resolution Airborne Wideband Camera. We derive magnetic field strength estimates using the Davis–Chandrasekhar–Fermi method. We compare the polarization and magnetic field strengths to column densities and dust continuum intensities across the region to build a coherent picture of the relationship between star-forming activity and magnetic fields in the region. The projected magnetic field strengths derived are in the range of ∼50–130 μG, which is typical for clouds of similar n(H2), i.e., molecular hydrogen volume density on the order of 104–105 cm‑3. We conclude that star formation occurs in the finger tips when the magnetic fields are too weak to prevent radial collapse due to gravity but strong enough to oppose OB stellar radiation pressure, while in the base of the fingers the magnetic fields hinder mass accretion and consequently star formation. We also support an initial weak-field model (<50 μG) with subsequent strengthening through realignment and compression, resulting in a dynamically important magnetic field.Fil: Sarkar, Adwitiya. University of Illinois at Urbana; Estados UnidosFil: Looney, Leslie W.. University of Illinois at Urbana; Estados UnidosFil: Pound, Marc W.. University of Maryland; Estados UnidosFil: Li, Zhi Yun. University of Virginia; Estados UnidosFil: Stephens, Ian W.. Worcester Polytechnic Institute; Estados UnidosFil: 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: Coudé, Simon. Worcester Polytechnic Institute; Estados UnidosFil: Lin, Zhe-Yu Daniel. University of Virginia; Estados UnidosFil: Yang, Haifeng. Zhejiang University; ChinaFil: Faistl, Reid. University of Illinois at Urbana; Estados UnidosIOP Publishing2025-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/278971Sarkar, Adwitiya; Looney, Leslie W.; Pound, Marc W.; Li, Zhi Yun; Stephens, Ian W.; et al.; Magnetic Fields in the Pillars of Creation; IOP Publishing; Astrophysical Journal; 988; 1; 7-2025; 1-110004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/ade544info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ade544info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2026-01-14T11:47:32Zoai:ri.conicet.gov.ar:11336/278971instacron: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:34982026-01-14 11:47:32.376CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Magnetic Fields in the Pillars of Creation
title Magnetic Fields in the Pillars of Creation
spellingShingle Magnetic Fields in the Pillars of Creation
Sarkar, Adwitiya
Polarimetry
Dust continuum emission
title_short Magnetic Fields in the Pillars of Creation
title_full Magnetic Fields in the Pillars of Creation
title_fullStr Magnetic Fields in the Pillars of Creation
title_full_unstemmed Magnetic Fields in the Pillars of Creation
title_sort Magnetic Fields in the Pillars of Creation
dc.creator.none.fl_str_mv Sarkar, Adwitiya
Looney, Leslie W.
Pound, Marc W.
Li, Zhi Yun
Stephens, Ian W.
Fernandez Lopez, Manuel
Coudé, Simon
Lin, Zhe-Yu Daniel
Yang, Haifeng
Faistl, Reid
author Sarkar, Adwitiya
author_facet Sarkar, Adwitiya
Looney, Leslie W.
Pound, Marc W.
Li, Zhi Yun
Stephens, Ian W.
Fernandez Lopez, Manuel
Coudé, Simon
Lin, Zhe-Yu Daniel
Yang, Haifeng
Faistl, Reid
author_role author
author2 Looney, Leslie W.
Pound, Marc W.
Li, Zhi Yun
Stephens, Ian W.
Fernandez Lopez, Manuel
Coudé, Simon
Lin, Zhe-Yu Daniel
Yang, Haifeng
Faistl, Reid
author2_role author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Polarimetry
Dust continuum emission
topic Polarimetry
Dust continuum emission
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Due to dust grain alignment with magnetic fields, dust polarization observations of far-infrared emission from cold molecular clouds are often used to trace magnetic fields, allowing a probe of the effects of magnetic fields on the star formation process. We present inferred magnetic field maps of the Pillars of Creation region within the larger M16 emission nebula, derived from dust polarization data in the 89 and 154 μm continuum using the Stratospheric Observatory For Infrared Astronomy/High-resolution Airborne Wideband Camera. We derive magnetic field strength estimates using the Davis–Chandrasekhar–Fermi method. We compare the polarization and magnetic field strengths to column densities and dust continuum intensities across the region to build a coherent picture of the relationship between star-forming activity and magnetic fields in the region. The projected magnetic field strengths derived are in the range of ∼50–130 μG, which is typical for clouds of similar n(H2), i.e., molecular hydrogen volume density on the order of 104–105 cm‑3. We conclude that star formation occurs in the finger tips when the magnetic fields are too weak to prevent radial collapse due to gravity but strong enough to oppose OB stellar radiation pressure, while in the base of the fingers the magnetic fields hinder mass accretion and consequently star formation. We also support an initial weak-field model (<50 μG) with subsequent strengthening through realignment and compression, resulting in a dynamically important magnetic field.
Fil: Sarkar, Adwitiya. University of Illinois at Urbana; Estados Unidos
Fil: Looney, Leslie W.. University of Illinois at Urbana; Estados Unidos
Fil: Pound, Marc W.. University of Maryland; Estados Unidos
Fil: Li, Zhi Yun. University of Virginia; Estados Unidos
Fil: Stephens, Ian W.. Worcester Polytechnic Institute; Estados Unidos
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: Coudé, Simon. Worcester Polytechnic Institute; Estados Unidos
Fil: Lin, Zhe-Yu Daniel. University of Virginia; Estados Unidos
Fil: Yang, Haifeng. Zhejiang University; China
Fil: Faistl, Reid. University of Illinois at Urbana; Estados Unidos
description Due to dust grain alignment with magnetic fields, dust polarization observations of far-infrared emission from cold molecular clouds are often used to trace magnetic fields, allowing a probe of the effects of magnetic fields on the star formation process. We present inferred magnetic field maps of the Pillars of Creation region within the larger M16 emission nebula, derived from dust polarization data in the 89 and 154 μm continuum using the Stratospheric Observatory For Infrared Astronomy/High-resolution Airborne Wideband Camera. We derive magnetic field strength estimates using the Davis–Chandrasekhar–Fermi method. We compare the polarization and magnetic field strengths to column densities and dust continuum intensities across the region to build a coherent picture of the relationship between star-forming activity and magnetic fields in the region. The projected magnetic field strengths derived are in the range of ∼50–130 μG, which is typical for clouds of similar n(H2), i.e., molecular hydrogen volume density on the order of 104–105 cm‑3. We conclude that star formation occurs in the finger tips when the magnetic fields are too weak to prevent radial collapse due to gravity but strong enough to oppose OB stellar radiation pressure, while in the base of the fingers the magnetic fields hinder mass accretion and consequently star formation. We also support an initial weak-field model (<50 μG) with subsequent strengthening through realignment and compression, resulting in a dynamically important magnetic field.
publishDate 2025
dc.date.none.fl_str_mv 2025-07
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/11336/278971
Sarkar, Adwitiya; Looney, Leslie W.; Pound, Marc W.; Li, Zhi Yun; Stephens, Ian W.; et al.; Magnetic Fields in the Pillars of Creation; IOP Publishing; Astrophysical Journal; 988; 1; 7-2025; 1-11
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/278971
identifier_str_mv Sarkar, Adwitiya; Looney, Leslie W.; Pound, Marc W.; Li, Zhi Yun; Stephens, Ian W.; et al.; Magnetic Fields in the Pillars of Creation; IOP Publishing; Astrophysical Journal; 988; 1; 7-2025; 1-11
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/ade544
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/ade544
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
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score 13.211636

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