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.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto Argentino de Radioastronomía
Materia
Ciencias Astronómicas
ISM: individual objects: G272.2-3.2
ISM: supernova remnants
Radiation mechanisms: thermal
X-rays: ISM
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/85504

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repository_id_str 1329
network_name_str SEDICI (UNLP)
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.Ciencias AstronómicasISM: individual objects: G272.2-3.2ISM: supernova remnantsRadiation mechanisms: thermalX-rays: ISMAims. 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 <i>XMM-Newton</i> and <i>Chandra images</i>, 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.Facultad de Ciencias Astronómicas y GeofísicasInstituto Argentino de Radioastronomía2013info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/85504enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201219709info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:16:30Zoai:sedici.unlp.edu.ar:10915/85504Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:31.077SEDICI (UNLP) - Universidad Nacional de La Platafalse
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.
Ciencias Astronómicas
ISM: individual objects: G272.2-3.2
ISM: supernova remnants
Radiation mechanisms: thermal
X-rays: ISM
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 Ciencias Astronómicas
ISM: individual objects: G272.2-3.2
ISM: supernova remnants
Radiation mechanisms: thermal
X-rays: ISM
topic Ciencias Astronómicas
ISM: individual objects: G272.2-3.2
ISM: supernova remnants
Radiation mechanisms: thermal
X-rays: ISM
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 <i>XMM-Newton</i> and <i>Chandra images</i>, 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.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto Argentino de Radioastronomía
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 <i>XMM-Newton</i> and <i>Chandra images</i>, 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
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
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info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201219709
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Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
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rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
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