XMM-Newton and Chandra observations of G272.2-3.2. Evidence of stellar ejecta in the central region

Autores
Sánchez Ayaso, E.; Combi, Jorge Ariel; Bocchino, F.; Albacete Colombo, Juan Facundo; López-santiago, J.; Martí, J.; Castro, E.
Año de publicación
2013
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Aims. We aim to study the spatial distribution of the physical and chemical properties of the X-ray emitting plasma of the supernova remnant G272.2−3.2 in order to obtain important constraints on its ionization stage, the progenitor supernova explosion, and the age of the remnant. Methods. We report on combined XMM-Newton and Chandra images, median photon energy maps, silicon and sulfur equivalent width maps, and a spatially resolved spectral analysis for a set of regions of the remnant. Complementary radio and Hα observations, available in the literature, are also used to study the multi-wavelength connection of all detected emissions. Results. The X-ray morphology of the remnant displays an overall structure with an almost circular appearance and a centrally brightened hard region with a peculiar elongated hard structure oriented along the northwest-southeast direction of the central part. The X-ray spectral study of the regions shows distinct Kα emission-line features of metal elements, confirming the thermal origin of the emission. The X-ray spectra are well represented by an absorbed variable abundance non-equilibrium ionization thermal plasma model, which produces elevated abundances of Si, S, and Fe in the circular central region, typical of ejecta material. The values of abundances found in the central region of the supernova remnant favor a Type Ia progenitor for this remnant. The outer region shows abundances below the solar value, to be expected if the emission arises from the shocked interstellar medium. The relatively low ionization timescales suggest non-equilibrium ionization. We identify the location of the contact discontinuity. Its distance to the outer shock is higher than expected for expansion in a uniform media, which suggests that the remnant spent most of its time in more dense medium.
Fil: Sánchez Ayaso, E.. Universidad de Jaén; España
Fil: Combi, Jorge Ariel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto Argentino de Radioastronomia (i); Argentina
Fil: Bocchino, F.. Istituto Nazionale Di Astrofisica; Italia
Fil: Albacete Colombo, Juan Facundo. Universidad Nacional del Comahue; Argentina
Fil: López-santiago, J.. Universidad Complutense de Madrid; España
Fil: Martí, J.. Universidad de Jaén; España
Fil: Castro, E.. Universidad de Jaén; España
Materia
ISM: SUPERNOVA REMNANTS
X-RAYS: ISM
RADIATION MECHANISMS: THERMAL
ISM: INDIVIDUAL OBJECTS: G272.2-3.2
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:11336/2641
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/2641
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling XMM-Newton and Chandra observations of G272.2-3.2. Evidence of stellar ejecta in the central regionSánchez Ayaso, E.Combi, Jorge ArielBocchino, F.Albacete Colombo, Juan FacundoLópez-santiago, J.Martí, J.Castro, E.ISM: SUPERNOVA REMNANTSX-RAYS: ISMRADIATION MECHANISMS: THERMALISM: INDIVIDUAL OBJECTS: G272.2-3.2https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Aims. We aim to study the spatial distribution of the physical and chemical properties of the X-ray emitting plasma of the supernova remnant G272.2−3.2 in order to obtain important constraints on its ionization stage, the progenitor supernova explosion, and the age of the remnant. Methods. We report on combined XMM-Newton and Chandra images, median photon energy maps, silicon and sulfur equivalent width maps, and a spatially resolved spectral analysis for a set of regions of the remnant. Complementary radio and Hα observations, available in the literature, are also used to study the multi-wavelength connection of all detected emissions. Results. The X-ray morphology of the remnant displays an overall structure with an almost circular appearance and a centrally brightened hard region with a peculiar elongated hard structure oriented along the northwest-southeast direction of the central part. The X-ray spectral study of the regions shows distinct Kα emission-line features of metal elements, confirming the thermal origin of the emission. The X-ray spectra are well represented by an absorbed variable abundance non-equilibrium ionization thermal plasma model, which produces elevated abundances of Si, S, and Fe in the circular central region, typical of ejecta material. The values of abundances found in the central region of the supernova remnant favor a Type Ia progenitor for this remnant. The outer region shows abundances below the solar value, to be expected if the emission arises from the shocked interstellar medium. The relatively low ionization timescales suggest non-equilibrium ionization. We identify the location of the contact discontinuity. Its distance to the outer shock is higher than expected for expansion in a uniform media, which suggests that the remnant spent most of its time in more dense medium.Fil: Sánchez Ayaso, E.. Universidad de Jaén; EspañaFil: Combi, Jorge Ariel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto Argentino de Radioastronomia (i); ArgentinaFil: Bocchino, F.. Istituto Nazionale Di Astrofisica; ItaliaFil: Albacete Colombo, Juan Facundo. Universidad Nacional del Comahue; ArgentinaFil: López-santiago, J.. Universidad Complutense de Madrid; EspañaFil: Martí, J.. Universidad de Jaén; EspañaFil: Castro, E.. Universidad de Jaén; EspañaEdp Sciences2013-03-22info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/2641Sánchez Ayaso, E.; Combi, Jorge Ariel; Bocchino, F.; Albacete Colombo, Juan Facundo; López-santiago, J.; et al.; XMM-Newton and Chandra observations of G272.2-3.2. Evidence of stellar ejecta in the central region; Edp Sciences; Astronomy And Astrophysics; 552; A52; 22-3-2013; 1-90004-63611432-0746enginfo:eu-repo/semantics/altIdentifier/doi/info:eu-repo/semantics/altIdentifier/arxiv/1301.1507info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201219709info:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/abs/2013A%26A...552A..52Sinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:44:30Zoai:ri.conicet.gov.ar:11336/2641instacron: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 11:44:31.163CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv XMM-Newton and Chandra observations of G272.2-3.2. Evidence of stellar ejecta in the central region
title XMM-Newton and Chandra observations of G272.2-3.2. Evidence of stellar ejecta in the central region
spellingShingle XMM-Newton and Chandra observations of G272.2-3.2. Evidence of stellar ejecta in the central region
Sánchez Ayaso, E.
ISM: SUPERNOVA REMNANTS
X-RAYS: ISM
RADIATION MECHANISMS: THERMAL
ISM: INDIVIDUAL OBJECTS: G272.2-3.2
title_short XMM-Newton and Chandra observations of G272.2-3.2. Evidence of stellar ejecta in the central region
title_full XMM-Newton and Chandra observations of G272.2-3.2. Evidence of stellar ejecta in the central region
title_fullStr XMM-Newton and Chandra observations of G272.2-3.2. Evidence of stellar ejecta in the central region
title_full_unstemmed XMM-Newton and Chandra observations of G272.2-3.2. Evidence of stellar ejecta in the central region
title_sort XMM-Newton and Chandra observations of G272.2-3.2. Evidence of stellar ejecta in the central region
dc.creator.none.fl_str_mv Sánchez Ayaso, E.
Combi, Jorge Ariel
Bocchino, F.
Albacete Colombo, Juan Facundo
López-santiago, J.
Martí, J.
Castro, E.
author Sánchez Ayaso, E.
author_facet Sánchez Ayaso, E.
Combi, Jorge Ariel
Bocchino, F.
Albacete Colombo, Juan Facundo
López-santiago, J.
Martí, J.
Castro, E.
author_role author
author2 Combi, Jorge Ariel
Bocchino, F.
Albacete Colombo, Juan Facundo
López-santiago, J.
Martí, J.
Castro, E.
author2_role author
author
author
author
author
author
dc.subject.none.fl_str_mv ISM: SUPERNOVA REMNANTS
X-RAYS: ISM
RADIATION MECHANISMS: THERMAL
ISM: INDIVIDUAL OBJECTS: G272.2-3.2
topic ISM: SUPERNOVA REMNANTS
X-RAYS: ISM
RADIATION MECHANISMS: THERMAL
ISM: INDIVIDUAL OBJECTS: G272.2-3.2
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Aims. We aim to study the spatial distribution of the physical and chemical properties of the X-ray emitting plasma of the supernova remnant G272.2−3.2 in order to obtain important constraints on its ionization stage, the progenitor supernova explosion, and the age of the remnant. Methods. We report on combined XMM-Newton and Chandra images, median photon energy maps, silicon and sulfur equivalent width maps, and a spatially resolved spectral analysis for a set of regions of the remnant. Complementary radio and Hα observations, available in the literature, are also used to study the multi-wavelength connection of all detected emissions. Results. The X-ray morphology of the remnant displays an overall structure with an almost circular appearance and a centrally brightened hard region with a peculiar elongated hard structure oriented along the northwest-southeast direction of the central part. The X-ray spectral study of the regions shows distinct Kα emission-line features of metal elements, confirming the thermal origin of the emission. The X-ray spectra are well represented by an absorbed variable abundance non-equilibrium ionization thermal plasma model, which produces elevated abundances of Si, S, and Fe in the circular central region, typical of ejecta material. The values of abundances found in the central region of the supernova remnant favor a Type Ia progenitor for this remnant. The outer region shows abundances below the solar value, to be expected if the emission arises from the shocked interstellar medium. The relatively low ionization timescales suggest non-equilibrium ionization. We identify the location of the contact discontinuity. Its distance to the outer shock is higher than expected for expansion in a uniform media, which suggests that the remnant spent most of its time in more dense medium.
Fil: Sánchez Ayaso, E.. Universidad de Jaén; España
Fil: Combi, Jorge Ariel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto Argentino de Radioastronomia (i); Argentina
Fil: Bocchino, F.. Istituto Nazionale Di Astrofisica; Italia
Fil: Albacete Colombo, Juan Facundo. Universidad Nacional del Comahue; Argentina
Fil: López-santiago, J.. Universidad Complutense de Madrid; España
Fil: Martí, J.. Universidad de Jaén; España
Fil: Castro, E.. Universidad de Jaén; España
description Aims. We aim to study the spatial distribution of the physical and chemical properties of the X-ray emitting plasma of the supernova remnant G272.2−3.2 in order to obtain important constraints on its ionization stage, the progenitor supernova explosion, and the age of the remnant. Methods. We report on combined XMM-Newton and Chandra images, median photon energy maps, silicon and sulfur equivalent width maps, and a spatially resolved spectral analysis for a set of regions of the remnant. Complementary radio and Hα observations, available in the literature, are also used to study the multi-wavelength connection of all detected emissions. Results. The X-ray morphology of the remnant displays an overall structure with an almost circular appearance and a centrally brightened hard region with a peculiar elongated hard structure oriented along the northwest-southeast direction of the central part. The X-ray spectral study of the regions shows distinct Kα emission-line features of metal elements, confirming the thermal origin of the emission. The X-ray spectra are well represented by an absorbed variable abundance non-equilibrium ionization thermal plasma model, which produces elevated abundances of Si, S, and Fe in the circular central region, typical of ejecta material. The values of abundances found in the central region of the supernova remnant favor a Type Ia progenitor for this remnant. The outer region shows abundances below the solar value, to be expected if the emission arises from the shocked interstellar medium. The relatively low ionization timescales suggest non-equilibrium ionization. We identify the location of the contact discontinuity. Its distance to the outer shock is higher than expected for expansion in a uniform media, which suggests that the remnant spent most of its time in more dense medium.
publishDate 2013
dc.date.none.fl_str_mv 2013-03-22
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/11336/2641
Sánchez Ayaso, E.; Combi, Jorge Ariel; Bocchino, F.; Albacete Colombo, Juan Facundo; López-santiago, J.; et al.; XMM-Newton and Chandra observations of G272.2-3.2. Evidence of stellar ejecta in the central region; Edp Sciences; Astronomy And Astrophysics; 552; A52; 22-3-2013; 1-9
0004-6361
1432-0746
url http://hdl.handle.net/11336/2641
identifier_str_mv Sánchez Ayaso, E.; Combi, Jorge Ariel; Bocchino, F.; Albacete Colombo, Juan Facundo; López-santiago, J.; et al.; XMM-Newton and Chandra observations of G272.2-3.2. Evidence of stellar ejecta in the central region; Edp Sciences; Astronomy And Astrophysics; 552; A52; 22-3-2013; 1-9
0004-6361
1432-0746
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/
info:eu-repo/semantics/altIdentifier/arxiv/1301.1507
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201219709
info:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/abs/2013A%26A...552A..52S
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 Edp Sciences
publisher.none.fl_str_mv Edp Sciences
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 12.982451

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