The VMC Survey. XXVII. Young Stellar Structures in the LMC's Bar Star-forming Complex

Autores
Sun, Ning-Chen; Grijs, Richard De; Subramanian, Smitha; Bekki, Kenji; Bell, Cameron P. M.; Cioni, Maria-Rosa L.; Ivanov, Valentin D.; Marconi, Marcella; Oliveira, Joana M.; Piatti, Andres Eduardo; Ripepi, Vincenzo; Rubele, Stefano; Tatton, Ben L.; Loon, Jacco Th. Van
Año de publicación
2017
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Star formation is a hierarchical process, forming young stellar structures of star clusters, associations, and complexes over a wide range of scales. The star-forming complex in the bar region of the Large Magellanic Cloud is investigated with upper main-sequence stars observed by the VISTA Survey of the Magellanic Clouds. The upper main-sequence stars exhibit highly nonuniform distributions. Young stellar structures inside the complex are identified from the stellar density map as density enhancements of different significance levels. We find that these structures are hierarchically organized such that larger, lower-density structures contain one or several smaller, higher-density ones. They follow power-law size and mass distributions, as well as a lognormal surface density distribution. All these results support a scenario of hierarchical star formation regulated by turbulence. The temporal evolution of young stellar structures is explored by using subsamples of upper main-sequence stars with different magnitude and age ranges. While the youngest subsample, with a median age of log(τ/yr) = 7.2, contains the most substructure, progressively older ones are less and less substructured. The oldest subsample, with a median age of log(τ/yr) = 8.0, is almost indistinguishable from a uniform distribution on spatial scales of 30-300 pc, suggesting that the young stellar structures are completely dispersed on a timescale of ∼100 Myr. These results are consistent with the characteristics of the 30 Doradus complex and the entire Large Magellanic Cloud, suggesting no significant environmental effects. We further point out that the fractal dimension may be method dependent for stellar samples with significant age spreads.
Fil: Sun, Ning-Chen. Peking University; China. International Space Science Institute; China
Fil: Grijs, Richard De. International Space Science Institute; China. Peking University; China
Fil: Subramanian, Smitha. Peking University; China
Fil: Bekki, Kenji. University of Western Australia; Australia
Fil: Bell, Cameron P. M.. Universita Zu Berlin. Universita Postdam; Alemania. Astrophysikalisches Institut Potsdam; Alemania
Fil: Cioni, Maria-Rosa L.. Universita Zu Berlin. Universita Postdam; Alemania. University Of Hertfordshire; Reino Unido. Astrophysikalisches Institut Potsdam; Alemania
Fil: Ivanov, Valentin D.. European Southern Observatory; Chile
Fil: Marconi, Marcella. Osservatorio Astronomico Di Capodimonte; Italia
Fil: Oliveira, Joana M.. Keele University; Reino Unido
Fil: Piatti, Andres Eduardo. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; Argentina
Fil: Ripepi, Vincenzo. Osservatorio Astronomico Di Capodimonte; Italia. Keele University; Reino Unido
Fil: Rubele, Stefano. Università di Padova; Italia
Fil: Tatton, Ben L.. Keele University; Reino Unido
Fil: Loon, Jacco Th. Van. Keele University; Reino Unido
Materia
INFRARED: STARS
MAGELLANIC CLOUDS
STARS: 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:11336/72213
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/72213
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The VMC Survey. XXVII. Young Stellar Structures in the LMC's Bar Star-forming ComplexSun, Ning-ChenGrijs, Richard DeSubramanian, SmithaBekki, KenjiBell, Cameron P. M.Cioni, Maria-Rosa L.Ivanov, Valentin D.Marconi, MarcellaOliveira, Joana M.Piatti, Andres EduardoRipepi, VincenzoRubele, StefanoTatton, Ben L.Loon, Jacco Th. VanINFRARED: STARSMAGELLANIC CLOUDSSTARS: FORMATIONStar formation is a hierarchical process, forming young stellar structures of star clusters, associations, and complexes over a wide range of scales. The star-forming complex in the bar region of the Large Magellanic Cloud is investigated with upper main-sequence stars observed by the VISTA Survey of the Magellanic Clouds. The upper main-sequence stars exhibit highly nonuniform distributions. Young stellar structures inside the complex are identified from the stellar density map as density enhancements of different significance levels. We find that these structures are hierarchically organized such that larger, lower-density structures contain one or several smaller, higher-density ones. They follow power-law size and mass distributions, as well as a lognormal surface density distribution. All these results support a scenario of hierarchical star formation regulated by turbulence. The temporal evolution of young stellar structures is explored by using subsamples of upper main-sequence stars with different magnitude and age ranges. While the youngest subsample, with a median age of log(τ/yr) = 7.2, contains the most substructure, progressively older ones are less and less substructured. The oldest subsample, with a median age of log(τ/yr) = 8.0, is almost indistinguishable from a uniform distribution on spatial scales of 30-300 pc, suggesting that the young stellar structures are completely dispersed on a timescale of ∼100 Myr. These results are consistent with the characteristics of the 30 Doradus complex and the entire Large Magellanic Cloud, suggesting no significant environmental effects. We further point out that the fractal dimension may be method dependent for stellar samples with significant age spreads.Fil: Sun, Ning-Chen. Peking University; China. International Space Science Institute; ChinaFil: Grijs, Richard De. International Space Science Institute; China. Peking University; ChinaFil: Subramanian, Smitha. Peking University; ChinaFil: Bekki, Kenji. University of Western Australia; AustraliaFil: Bell, Cameron P. M.. Universita Zu Berlin. Universita Postdam; Alemania. Astrophysikalisches Institut Potsdam; AlemaniaFil: Cioni, Maria-Rosa L.. Universita Zu Berlin. Universita Postdam; Alemania. University Of Hertfordshire; Reino Unido. Astrophysikalisches Institut Potsdam; AlemaniaFil: Ivanov, Valentin D.. European Southern Observatory; ChileFil: Marconi, Marcella. Osservatorio Astronomico Di Capodimonte; ItaliaFil: Oliveira, Joana M.. Keele University; Reino UnidoFil: Piatti, Andres Eduardo. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; ArgentinaFil: Ripepi, Vincenzo. Osservatorio Astronomico Di Capodimonte; Italia. Keele University; Reino UnidoFil: Rubele, Stefano. Università di Padova; ItaliaFil: Tatton, Ben L.. Keele University; Reino UnidoFil: Loon, Jacco Th. Van. Keele University; Reino UnidoIOP Publishing2017-11info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/72213Sun, Ning-Chen; Grijs, Richard De; Subramanian, Smitha; Bekki, Kenji; Bell, Cameron P. M.; et al.; The VMC Survey. XXVII. Young Stellar Structures in the LMC's Bar Star-forming Complex; IOP Publishing; Astrophysical Journal; 849; 2; 11-20170004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.3847/1538-4357/aa911e/metainfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aa911einfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:19:25Zoai:ri.conicet.gov.ar:11336/72213instacron: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 10:19:26.185CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The VMC Survey. XXVII. Young Stellar Structures in the LMC's Bar Star-forming Complex
title The VMC Survey. XXVII. Young Stellar Structures in the LMC's Bar Star-forming Complex
spellingShingle The VMC Survey. XXVII. Young Stellar Structures in the LMC's Bar Star-forming Complex
Sun, Ning-Chen
INFRARED: STARS
MAGELLANIC CLOUDS
STARS: FORMATION
title_short The VMC Survey. XXVII. Young Stellar Structures in the LMC's Bar Star-forming Complex
title_full The VMC Survey. XXVII. Young Stellar Structures in the LMC's Bar Star-forming Complex
title_fullStr The VMC Survey. XXVII. Young Stellar Structures in the LMC's Bar Star-forming Complex
title_full_unstemmed The VMC Survey. XXVII. Young Stellar Structures in the LMC's Bar Star-forming Complex
title_sort The VMC Survey. XXVII. Young Stellar Structures in the LMC's Bar Star-forming Complex
dc.creator.none.fl_str_mv Sun, Ning-Chen
Grijs, Richard De
Subramanian, Smitha
Bekki, Kenji
Bell, Cameron P. M.
Cioni, Maria-Rosa L.
Ivanov, Valentin D.
Marconi, Marcella
Oliveira, Joana M.
Piatti, Andres Eduardo
Ripepi, Vincenzo
Rubele, Stefano
Tatton, Ben L.
Loon, Jacco Th. Van
author Sun, Ning-Chen
author_facet Sun, Ning-Chen
Grijs, Richard De
Subramanian, Smitha
Bekki, Kenji
Bell, Cameron P. M.
Cioni, Maria-Rosa L.
Ivanov, Valentin D.
Marconi, Marcella
Oliveira, Joana M.
Piatti, Andres Eduardo
Ripepi, Vincenzo
Rubele, Stefano
Tatton, Ben L.
Loon, Jacco Th. Van
author_role author
author2 Grijs, Richard De
Subramanian, Smitha
Bekki, Kenji
Bell, Cameron P. M.
Cioni, Maria-Rosa L.
Ivanov, Valentin D.
Marconi, Marcella
Oliveira, Joana M.
Piatti, Andres Eduardo
Ripepi, Vincenzo
Rubele, Stefano
Tatton, Ben L.
Loon, Jacco Th. Van
author2_role author
author
author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv INFRARED: STARS
MAGELLANIC CLOUDS
STARS: FORMATION
topic INFRARED: STARS
MAGELLANIC CLOUDS
STARS: FORMATION
dc.description.none.fl_txt_mv Star formation is a hierarchical process, forming young stellar structures of star clusters, associations, and complexes over a wide range of scales. The star-forming complex in the bar region of the Large Magellanic Cloud is investigated with upper main-sequence stars observed by the VISTA Survey of the Magellanic Clouds. The upper main-sequence stars exhibit highly nonuniform distributions. Young stellar structures inside the complex are identified from the stellar density map as density enhancements of different significance levels. We find that these structures are hierarchically organized such that larger, lower-density structures contain one or several smaller, higher-density ones. They follow power-law size and mass distributions, as well as a lognormal surface density distribution. All these results support a scenario of hierarchical star formation regulated by turbulence. The temporal evolution of young stellar structures is explored by using subsamples of upper main-sequence stars with different magnitude and age ranges. While the youngest subsample, with a median age of log(τ/yr) = 7.2, contains the most substructure, progressively older ones are less and less substructured. The oldest subsample, with a median age of log(τ/yr) = 8.0, is almost indistinguishable from a uniform distribution on spatial scales of 30-300 pc, suggesting that the young stellar structures are completely dispersed on a timescale of ∼100 Myr. These results are consistent with the characteristics of the 30 Doradus complex and the entire Large Magellanic Cloud, suggesting no significant environmental effects. We further point out that the fractal dimension may be method dependent for stellar samples with significant age spreads.
Fil: Sun, Ning-Chen. Peking University; China. International Space Science Institute; China
Fil: Grijs, Richard De. International Space Science Institute; China. Peking University; China
Fil: Subramanian, Smitha. Peking University; China
Fil: Bekki, Kenji. University of Western Australia; Australia
Fil: Bell, Cameron P. M.. Universita Zu Berlin. Universita Postdam; Alemania. Astrophysikalisches Institut Potsdam; Alemania
Fil: Cioni, Maria-Rosa L.. Universita Zu Berlin. Universita Postdam; Alemania. University Of Hertfordshire; Reino Unido. Astrophysikalisches Institut Potsdam; Alemania
Fil: Ivanov, Valentin D.. European Southern Observatory; Chile
Fil: Marconi, Marcella. Osservatorio Astronomico Di Capodimonte; Italia
Fil: Oliveira, Joana M.. Keele University; Reino Unido
Fil: Piatti, Andres Eduardo. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; Argentina
Fil: Ripepi, Vincenzo. Osservatorio Astronomico Di Capodimonte; Italia. Keele University; Reino Unido
Fil: Rubele, Stefano. Università di Padova; Italia
Fil: Tatton, Ben L.. Keele University; Reino Unido
Fil: Loon, Jacco Th. Van. Keele University; Reino Unido
description Star formation is a hierarchical process, forming young stellar structures of star clusters, associations, and complexes over a wide range of scales. The star-forming complex in the bar region of the Large Magellanic Cloud is investigated with upper main-sequence stars observed by the VISTA Survey of the Magellanic Clouds. The upper main-sequence stars exhibit highly nonuniform distributions. Young stellar structures inside the complex are identified from the stellar density map as density enhancements of different significance levels. We find that these structures are hierarchically organized such that larger, lower-density structures contain one or several smaller, higher-density ones. They follow power-law size and mass distributions, as well as a lognormal surface density distribution. All these results support a scenario of hierarchical star formation regulated by turbulence. The temporal evolution of young stellar structures is explored by using subsamples of upper main-sequence stars with different magnitude and age ranges. While the youngest subsample, with a median age of log(τ/yr) = 7.2, contains the most substructure, progressively older ones are less and less substructured. The oldest subsample, with a median age of log(τ/yr) = 8.0, is almost indistinguishable from a uniform distribution on spatial scales of 30-300 pc, suggesting that the young stellar structures are completely dispersed on a timescale of ∼100 Myr. These results are consistent with the characteristics of the 30 Doradus complex and the entire Large Magellanic Cloud, suggesting no significant environmental effects. We further point out that the fractal dimension may be method dependent for stellar samples with significant age spreads.
publishDate 2017
dc.date.none.fl_str_mv 2017-11
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/11336/72213
Sun, Ning-Chen; Grijs, Richard De; Subramanian, Smitha; Bekki, Kenji; Bell, Cameron P. M.; et al.; The VMC Survey. XXVII. Young Stellar Structures in the LMC's Bar Star-forming Complex; IOP Publishing; Astrophysical Journal; 849; 2; 11-2017
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/72213
identifier_str_mv Sun, Ning-Chen; Grijs, Richard De; Subramanian, Smitha; Bekki, Kenji; Bell, Cameron P. M.; et al.; The VMC Survey. XXVII. Young Stellar Structures in the LMC's Bar Star-forming Complex; IOP Publishing; Astrophysical Journal; 849; 2; 11-2017
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/aa911e/meta
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aa911e
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 13.070432

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