A comprehensive study of NGC 2023 with XMM–Newton and Spitzer
- Autores
- López García, M. A.; López Santiago, J.; Albacete Colombo, Juan Facundo; Pérez Gónzalez, P. G.; de Castro, E.
- Año de publicación
- 2013
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Nearby star-forming regions are ideal laboratories to study high-energy emission of different stellar populations, from very massive stars to brown dwarfs. NGC 2023 is a reflection nebula situated to the south of the Flame Nebula (NGC 2024) and at the edge of the H II region IC 434, which also contains the Horsehead Nebula (Barnard 33). NGC 2023, NGC 2024, Barnard 33 and the surroundings of the O-type supergiant star ζ Ori constitute the south part of the Orion B molecular complex. In this work, we present a comprehensive study of X-ray emitters in the region of NGC 2023 and its surroundings. We combine optical and infrared data to determine physical properties (mass, temperature, luminosity and the presence of accretion discs) of the stars detected in an XMM–Newton observation. This study has allowed us to analyse spectral energy distribution of these stars for the first time and determine their evolutionary stage. Properties of the X-ray emitting plasma of these stars are compared to those found in other nearby star-forming regions. The results indicate that the stars that are being formed in this region have characteristics, in terms of physical properties and luminosity function, similar to those found in the Taurus–Auriga molecular complex.
Fil: López García, M. A.. Universidad Complutense de Madrid; España
Fil: López Santiago, J.. Universidad Complutense de Madrid; España
Fil: Albacete Colombo, Juan Facundo. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional del Comahue. Centro Universidad Región Zona Atlántica; Argentina
Fil: Pérez Gónzalez, P. G. . Universidad Complutense de Madrid; España
Fil: de Castro, E.. Universidad Complutense de Madrid; España - Materia
-
STARS: CORONAE
STARS: PRE-MAIN-SEQUENCE
OPEN CLUSTERS AND ASSOCIATIONS: GENERAL
X-RAYS: STARS - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/11040
Ver los metadatos del registro completo
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A comprehensive study of NGC 2023 with XMM–Newton and SpitzerLópez García, M. A.López Santiago, J.Albacete Colombo, Juan FacundoPérez Gónzalez, P. G. de Castro, E.STARS: CORONAESTARS: PRE-MAIN-SEQUENCEOPEN CLUSTERS AND ASSOCIATIONS: GENERALX-RAYS: STARShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Nearby star-forming regions are ideal laboratories to study high-energy emission of different stellar populations, from very massive stars to brown dwarfs. NGC 2023 is a reflection nebula situated to the south of the Flame Nebula (NGC 2024) and at the edge of the H II region IC 434, which also contains the Horsehead Nebula (Barnard 33). NGC 2023, NGC 2024, Barnard 33 and the surroundings of the O-type supergiant star ζ Ori constitute the south part of the Orion B molecular complex. In this work, we present a comprehensive study of X-ray emitters in the region of NGC 2023 and its surroundings. We combine optical and infrared data to determine physical properties (mass, temperature, luminosity and the presence of accretion discs) of the stars detected in an XMM–Newton observation. This study has allowed us to analyse spectral energy distribution of these stars for the first time and determine their evolutionary stage. Properties of the X-ray emitting plasma of these stars are compared to those found in other nearby star-forming regions. The results indicate that the stars that are being formed in this region have characteristics, in terms of physical properties and luminosity function, similar to those found in the Taurus–Auriga molecular complex.Fil: López García, M. A.. Universidad Complutense de Madrid; EspañaFil: López Santiago, J.. Universidad Complutense de Madrid; EspañaFil: Albacete Colombo, Juan Facundo. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional del Comahue. Centro Universidad Región Zona Atlántica; ArgentinaFil: Pérez Gónzalez, P. G. . Universidad Complutense de Madrid; EspañaFil: de Castro, E.. Universidad Complutense de Madrid; EspañaOxford University Press2013-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/11040López García, M. A.; López Santiago, J.; Albacete Colombo, Juan Facundo; Pérez Gónzalez, P. G. ; de Castro, E.; A comprehensive study of NGC 2023 with XMM–Newton and Spitzer; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 429; 1; 1-2013; 775-7910035-87111365-2966enginfo:eu-repo/semantics/altIdentifier/url/http://mnras.oxfordjournals.org/content/429/1/775info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/sts373info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:38:35Zoai:ri.conicet.gov.ar:11336/11040instacron: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 09:38:35.995CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
A comprehensive study of NGC 2023 with XMM–Newton and Spitzer |
title |
A comprehensive study of NGC 2023 with XMM–Newton and Spitzer |
spellingShingle |
A comprehensive study of NGC 2023 with XMM–Newton and Spitzer López García, M. A. STARS: CORONAE STARS: PRE-MAIN-SEQUENCE OPEN CLUSTERS AND ASSOCIATIONS: GENERAL X-RAYS: STARS |
title_short |
A comprehensive study of NGC 2023 with XMM–Newton and Spitzer |
title_full |
A comprehensive study of NGC 2023 with XMM–Newton and Spitzer |
title_fullStr |
A comprehensive study of NGC 2023 with XMM–Newton and Spitzer |
title_full_unstemmed |
A comprehensive study of NGC 2023 with XMM–Newton and Spitzer |
title_sort |
A comprehensive study of NGC 2023 with XMM–Newton and Spitzer |
dc.creator.none.fl_str_mv |
López García, M. A. López Santiago, J. Albacete Colombo, Juan Facundo Pérez Gónzalez, P. G. de Castro, E. |
author |
López García, M. A. |
author_facet |
López García, M. A. López Santiago, J. Albacete Colombo, Juan Facundo Pérez Gónzalez, P. G. de Castro, E. |
author_role |
author |
author2 |
López Santiago, J. Albacete Colombo, Juan Facundo Pérez Gónzalez, P. G. de Castro, E. |
author2_role |
author author author author |
dc.subject.none.fl_str_mv |
STARS: CORONAE STARS: PRE-MAIN-SEQUENCE OPEN CLUSTERS AND ASSOCIATIONS: GENERAL X-RAYS: STARS |
topic |
STARS: CORONAE STARS: PRE-MAIN-SEQUENCE OPEN CLUSTERS AND ASSOCIATIONS: GENERAL X-RAYS: STARS |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
Nearby star-forming regions are ideal laboratories to study high-energy emission of different stellar populations, from very massive stars to brown dwarfs. NGC 2023 is a reflection nebula situated to the south of the Flame Nebula (NGC 2024) and at the edge of the H II region IC 434, which also contains the Horsehead Nebula (Barnard 33). NGC 2023, NGC 2024, Barnard 33 and the surroundings of the O-type supergiant star ζ Ori constitute the south part of the Orion B molecular complex. In this work, we present a comprehensive study of X-ray emitters in the region of NGC 2023 and its surroundings. We combine optical and infrared data to determine physical properties (mass, temperature, luminosity and the presence of accretion discs) of the stars detected in an XMM–Newton observation. This study has allowed us to analyse spectral energy distribution of these stars for the first time and determine their evolutionary stage. Properties of the X-ray emitting plasma of these stars are compared to those found in other nearby star-forming regions. The results indicate that the stars that are being formed in this region have characteristics, in terms of physical properties and luminosity function, similar to those found in the Taurus–Auriga molecular complex. Fil: López García, M. A.. Universidad Complutense de Madrid; España Fil: López Santiago, J.. Universidad Complutense de Madrid; España Fil: Albacete Colombo, Juan Facundo. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional del Comahue. Centro Universidad Región Zona Atlántica; Argentina Fil: Pérez Gónzalez, P. G. . Universidad Complutense de Madrid; España Fil: de Castro, E.. Universidad Complutense de Madrid; España |
description |
Nearby star-forming regions are ideal laboratories to study high-energy emission of different stellar populations, from very massive stars to brown dwarfs. NGC 2023 is a reflection nebula situated to the south of the Flame Nebula (NGC 2024) and at the edge of the H II region IC 434, which also contains the Horsehead Nebula (Barnard 33). NGC 2023, NGC 2024, Barnard 33 and the surroundings of the O-type supergiant star ζ Ori constitute the south part of the Orion B molecular complex. In this work, we present a comprehensive study of X-ray emitters in the region of NGC 2023 and its surroundings. We combine optical and infrared data to determine physical properties (mass, temperature, luminosity and the presence of accretion discs) of the stars detected in an XMM–Newton observation. This study has allowed us to analyse spectral energy distribution of these stars for the first time and determine their evolutionary stage. Properties of the X-ray emitting plasma of these stars are compared to those found in other nearby star-forming regions. The results indicate that the stars that are being formed in this region have characteristics, in terms of physical properties and luminosity function, similar to those found in the Taurus–Auriga molecular complex. |
publishDate |
2013 |
dc.date.none.fl_str_mv |
2013-01 |
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/11336/11040 López García, M. A.; López Santiago, J.; Albacete Colombo, Juan Facundo; Pérez Gónzalez, P. G. ; de Castro, E.; A comprehensive study of NGC 2023 with XMM–Newton and Spitzer; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 429; 1; 1-2013; 775-791 0035-8711 1365-2966 |
url |
http://hdl.handle.net/11336/11040 |
identifier_str_mv |
López García, M. A.; López Santiago, J.; Albacete Colombo, Juan Facundo; Pérez Gónzalez, P. G. ; de Castro, E.; A comprehensive study of NGC 2023 with XMM–Newton and Spitzer; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 429; 1; 1-2013; 775-791 0035-8711 1365-2966 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/url/http://mnras.oxfordjournals.org/content/429/1/775 info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/sts373 |
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 |
Oxford University Press |
publisher.none.fl_str_mv |
Oxford University Press |
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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13.070432 |