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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/2641
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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 Técnicas2025-09-29T10:14:25Zoai: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:34982025-09-29 10:14:25.783CONICET 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 |
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Consejo Nacional de Investigaciones Científicas y Técnicas |
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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 |