Detailed study of SNR G306.3-0.9 using XMM-Newton and Chandra observations

Autores
Combi, Jorge Ariel; García, Federico; Suárez, Alejandra Etelvina; Luque Escamilla, Pedro; Paron, Sergio Ariel; Miceli, Marco
Año de publicación
2016
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 supernovaremnant (SNR) G306.3−0.9 in detail to obtain constraints on its ionization stage, the progenitor supernova explosion, and the age ofthe remnant.Methods. We used combined data from XMM-Newton and Chandra observatories to study the X-ray morphology of G306.3−0.9 in detail. A spatially resolved spectral analysis was used to obtain physical and geometrical parameters of different regions of the remnant. Spitzer infrared observations, available in the archive, were also used to constrain the progenitor supernova and study the environment in which the remnant evolved.Results. The X-ray morphology of the remnant displays a non-uniform structure of semi-circular appearance, with a bright southwest region and very weak or almost negligible X-ray emission in its northern part. These results indicate that the remnant is propagating in a non-uniform environment as the shock fronts are encountering a high-density medium, where enhanced infrared emission is detected. The X-ray spectral analysis of the selected regions shows distinct emission-line features of several metal elements, confirming the thermal origin of the emission. The X-ray spectra are well represented by a combination of two absorbed thermal plasma models: one in equilibrium ionization (VAPEC) with a mean temperature of ∼0.19 keV, and another out of equilibrium ionization (VNEI) at a higher temperature of ∼1.1 or 1.6?1.9 keV. For regions located in the northeast, central, and southwest part of the SNR, wefound elevated abundances of Si, S, Ar, Ca, and Fe, typical of ejecta material. The outer regions located northwest and south show values of the abundances above solar but lower than to those found in the central regions. This suggests that the composition of the emitting outer parts of the SNR is a combination of ejecta and shocked material of the interstellar medium. The comparison between the S/Si, Ar/Si, and Ca/Si abundances ratios (1.75, 1.27, and 2.72 in the central region, respectively), favor a Type Ia progenitor for this remnant, a result that is also supported by an independent morphological analysis using the X-ray and 24 µm IR data.
Fil: Combi, Jorge Ariel. Provincia de Buenos Aires. Gobernación. Comision de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomia; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: García, Federico. Provincia de Buenos Aires. Gobernación. Comision de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomia; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Suárez, Alejandra Etelvina. Provincia de Buenos Aires. Gobernación. Comision de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomia; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Luque Escamilla, Pedro. Universidad de Jaén; España
Fil: Paron, Sergio Ariel. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Miceli, Marco. Osservatorio Astronomico Di Palermo; Italia
Materia
ISM: individual objects: G306.3-0.9
ISM: supernova remnants
X-ray: ISM
radiation mechanism: thermal
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:11336/21900
Acceder
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network_name_str CONICET Digital (CONICET)
spelling Detailed study of SNR G306.3-0.9 using XMM-Newton and Chandra observationsCombi, Jorge ArielGarcía, FedericoSuárez, Alejandra EtelvinaLuque Escamilla, PedroParon, Sergio ArielMiceli, MarcoISM: individual objects: G306.3-0.9ISM: supernova remnantsX-ray: ISMradiation mechanism: thermalhttps://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 supernovaremnant (SNR) G306.3−0.9 in detail to obtain constraints on its ionization stage, the progenitor supernova explosion, and the age ofthe remnant.Methods. We used combined data from XMM-Newton and Chandra observatories to study the X-ray morphology of G306.3−0.9 in detail. A spatially resolved spectral analysis was used to obtain physical and geometrical parameters of different regions of the remnant. Spitzer infrared observations, available in the archive, were also used to constrain the progenitor supernova and study the environment in which the remnant evolved.Results. The X-ray morphology of the remnant displays a non-uniform structure of semi-circular appearance, with a bright southwest region and very weak or almost negligible X-ray emission in its northern part. These results indicate that the remnant is propagating in a non-uniform environment as the shock fronts are encountering a high-density medium, where enhanced infrared emission is detected. The X-ray spectral analysis of the selected regions shows distinct emission-line features of several metal elements, confirming the thermal origin of the emission. The X-ray spectra are well represented by a combination of two absorbed thermal plasma models: one in equilibrium ionization (VAPEC) with a mean temperature of ∼0.19 keV, and another out of equilibrium ionization (VNEI) at a higher temperature of ∼1.1 or 1.6?1.9 keV. For regions located in the northeast, central, and southwest part of the SNR, wefound elevated abundances of Si, S, Ar, Ca, and Fe, typical of ejecta material. The outer regions located northwest and south show values of the abundances above solar but lower than to those found in the central regions. This suggests that the composition of the emitting outer parts of the SNR is a combination of ejecta and shocked material of the interstellar medium. The comparison between the S/Si, Ar/Si, and Ca/Si abundances ratios (1.75, 1.27, and 2.72 in the central region, respectively), favor a Type Ia progenitor for this remnant, a result that is also supported by an independent morphological analysis using the X-ray and 24 µm IR data.Fil: Combi, Jorge Ariel. Provincia de Buenos Aires. Gobernación. Comision de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomia; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: García, Federico. Provincia de Buenos Aires. Gobernación. Comision de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomia; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Suárez, Alejandra Etelvina. Provincia de Buenos Aires. Gobernación. Comision de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomia; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Luque Escamilla, Pedro. Universidad de Jaén; EspañaFil: Paron, Sergio Ariel. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Miceli, Marco. Osservatorio Astronomico Di Palermo; ItaliaEDP Sciences2016-06info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/21900Combi, Jorge Ariel; García, Federico; Suárez, Alejandra Etelvina; Luque Escamilla, Pedro; Paron, Sergio Ariel; et al.; Detailed study of SNR G306.3-0.9 using XMM-Newton and Chandra observations; EDP Sciences; Astronomy and Astrophysics; 592; A125; 6-2016; 1-80004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201527014info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2016/08/aa27014-15/aa27014-15.htmlinfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/pdf/1606.08940.pdfinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:54:05Zoai:ri.conicet.gov.ar:11336/21900instacron: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 09:54:06.209CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Detailed study of SNR G306.3-0.9 using XMM-Newton and Chandra observations
title Detailed study of SNR G306.3-0.9 using XMM-Newton and Chandra observations
spellingShingle Detailed study of SNR G306.3-0.9 using XMM-Newton and Chandra observations
Combi, Jorge Ariel
ISM: individual objects: G306.3-0.9
ISM: supernova remnants
X-ray: ISM
radiation mechanism: thermal
title_short Detailed study of SNR G306.3-0.9 using XMM-Newton and Chandra observations
title_full Detailed study of SNR G306.3-0.9 using XMM-Newton and Chandra observations
title_fullStr Detailed study of SNR G306.3-0.9 using XMM-Newton and Chandra observations
title_full_unstemmed Detailed study of SNR G306.3-0.9 using XMM-Newton and Chandra observations
title_sort Detailed study of SNR G306.3-0.9 using XMM-Newton and Chandra observations
dc.creator.none.fl_str_mv Combi, Jorge Ariel
García, Federico
Suárez, Alejandra Etelvina
Luque Escamilla, Pedro
Paron, Sergio Ariel
Miceli, Marco
author Combi, Jorge Ariel
author_facet Combi, Jorge Ariel
García, Federico
Suárez, Alejandra Etelvina
Luque Escamilla, Pedro
Paron, Sergio Ariel
Miceli, Marco
author_role author
author2 García, Federico
Suárez, Alejandra Etelvina
Luque Escamilla, Pedro
Paron, Sergio Ariel
Miceli, Marco
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv ISM: individual objects: G306.3-0.9
ISM: supernova remnants
X-ray: ISM
radiation mechanism: thermal
topic ISM: individual objects: G306.3-0.9
ISM: supernova remnants
X-ray: ISM
radiation mechanism: thermal
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 supernovaremnant (SNR) G306.3−0.9 in detail to obtain constraints on its ionization stage, the progenitor supernova explosion, and the age ofthe remnant.Methods. We used combined data from XMM-Newton and Chandra observatories to study the X-ray morphology of G306.3−0.9 in detail. A spatially resolved spectral analysis was used to obtain physical and geometrical parameters of different regions of the remnant. Spitzer infrared observations, available in the archive, were also used to constrain the progenitor supernova and study the environment in which the remnant evolved.Results. The X-ray morphology of the remnant displays a non-uniform structure of semi-circular appearance, with a bright southwest region and very weak or almost negligible X-ray emission in its northern part. These results indicate that the remnant is propagating in a non-uniform environment as the shock fronts are encountering a high-density medium, where enhanced infrared emission is detected. The X-ray spectral analysis of the selected regions shows distinct emission-line features of several metal elements, confirming the thermal origin of the emission. The X-ray spectra are well represented by a combination of two absorbed thermal plasma models: one in equilibrium ionization (VAPEC) with a mean temperature of ∼0.19 keV, and another out of equilibrium ionization (VNEI) at a higher temperature of ∼1.1 or 1.6?1.9 keV. For regions located in the northeast, central, and southwest part of the SNR, wefound elevated abundances of Si, S, Ar, Ca, and Fe, typical of ejecta material. The outer regions located northwest and south show values of the abundances above solar but lower than to those found in the central regions. This suggests that the composition of the emitting outer parts of the SNR is a combination of ejecta and shocked material of the interstellar medium. The comparison between the S/Si, Ar/Si, and Ca/Si abundances ratios (1.75, 1.27, and 2.72 in the central region, respectively), favor a Type Ia progenitor for this remnant, a result that is also supported by an independent morphological analysis using the X-ray and 24 µm IR data.
Fil: Combi, Jorge Ariel. Provincia de Buenos Aires. Gobernación. Comision de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomia; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: García, Federico. Provincia de Buenos Aires. Gobernación. Comision de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomia; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Suárez, Alejandra Etelvina. Provincia de Buenos Aires. Gobernación. Comision de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomia; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Luque Escamilla, Pedro. Universidad de Jaén; España
Fil: Paron, Sergio Ariel. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Miceli, Marco. Osservatorio Astronomico Di Palermo; Italia
description Aims. We aim to study the spatial distribution of the physical and chemical properties of the X-ray emitting plasma of the supernovaremnant (SNR) G306.3−0.9 in detail to obtain constraints on its ionization stage, the progenitor supernova explosion, and the age ofthe remnant.Methods. We used combined data from XMM-Newton and Chandra observatories to study the X-ray morphology of G306.3−0.9 in detail. A spatially resolved spectral analysis was used to obtain physical and geometrical parameters of different regions of the remnant. Spitzer infrared observations, available in the archive, were also used to constrain the progenitor supernova and study the environment in which the remnant evolved.Results. The X-ray morphology of the remnant displays a non-uniform structure of semi-circular appearance, with a bright southwest region and very weak or almost negligible X-ray emission in its northern part. These results indicate that the remnant is propagating in a non-uniform environment as the shock fronts are encountering a high-density medium, where enhanced infrared emission is detected. The X-ray spectral analysis of the selected regions shows distinct emission-line features of several metal elements, confirming the thermal origin of the emission. The X-ray spectra are well represented by a combination of two absorbed thermal plasma models: one in equilibrium ionization (VAPEC) with a mean temperature of ∼0.19 keV, and another out of equilibrium ionization (VNEI) at a higher temperature of ∼1.1 or 1.6?1.9 keV. For regions located in the northeast, central, and southwest part of the SNR, wefound elevated abundances of Si, S, Ar, Ca, and Fe, typical of ejecta material. The outer regions located northwest and south show values of the abundances above solar but lower than to those found in the central regions. This suggests that the composition of the emitting outer parts of the SNR is a combination of ejecta and shocked material of the interstellar medium. The comparison between the S/Si, Ar/Si, and Ca/Si abundances ratios (1.75, 1.27, and 2.72 in the central region, respectively), favor a Type Ia progenitor for this remnant, a result that is also supported by an independent morphological analysis using the X-ray and 24 µm IR data.
publishDate 2016
dc.date.none.fl_str_mv 2016-06
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/11336/21900
Combi, Jorge Ariel; García, Federico; Suárez, Alejandra Etelvina; Luque Escamilla, Pedro; Paron, Sergio Ariel; et al.; Detailed study of SNR G306.3-0.9 using XMM-Newton and Chandra observations; EDP Sciences; Astronomy and Astrophysics; 592; A125; 6-2016; 1-8
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/21900
identifier_str_mv Combi, Jorge Ariel; García, Federico; Suárez, Alejandra Etelvina; Luque Escamilla, Pedro; Paron, Sergio Ariel; et al.; Detailed study of SNR G306.3-0.9 using XMM-Newton and Chandra observations; EDP Sciences; Astronomy and Astrophysics; 592; A125; 6-2016; 1-8
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201527014
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2016/08/aa27014-15/aa27014-15.html
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/pdf/1606.08940.pdf
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
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 13.070432

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