X-ray emitting structures in the Vela SNR: Ejecta anisotropies and progenitor stellar wind residuals

Autores
Sapienza, V.; Miceli, M.; Peres, G.; Bocchino, F.; Orlando, S.; Greco, E.; Combi, Jorge Ariel; García, Federico; Sasaki, M.
Año de publicación
2021
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. The Vela supernova remnant (SNR) shows several ejecta fragments (or shrapnel) protruding beyond the forward shock, which are most likely relics of anisotropies that developed during the supernova (SN) explosion. Recent studies have revealed high Si abundance in two shrapnel (shrapnel A and G), located in opposite directions with respect to the SNR center. This suggests the possible existence of a Si-rich jet-counterjet structure, similar to that observed in the SNR Cassiopea A. Aims. We analyzed an XMM-Newton observation of a bright clump, behind shrapnel G, which lies along the direction connecting shrapnel A and G. The aim is to study the physical and chemical properties of this clump to ascertain whether it is part of this putative jet-like structure. Methods. We produced background-corrected and adaptively-smoothed count-rate images and median photon energy maps, and performed a spatially resolved spectral analysis. Results. We identified two structures with different physical properties. The first one is remarkably elongated along the direction connecting shrapnel A and G. Its X-ray spectrum is much softer than that of the other two shrapnel, to the point of hindering the determination of the Si abundance; however, its physical and chemical properties are consistent with those of shrapnel A and shrapnel G. The second structure, running along the southeast-northwest direction, has a higher temperature and appears similar to a thin filament. By analyzing the ROSAT data, we have found that this filament is part of a very large and coherent structure that we identified in the western rim of the shell. Conclusions. We obtained a thorough description of the collimated, jet-like tail of shrapnel G in Vela SNR. In addition we discovered a coherent and very extended feature roughly perpendicular to the jet-like structure that we interpret as a signature of an earlier interaction of the remnant with the stellar wind of its progenitor star. The peculiar Ne/O ratio we found in the wind residual may be suggestive of a Wolf-Rayet progenitor for Vela SNR, though further analysis is required to address this point.
Fil: Sapienza, V.. Istituto Nazionale di Astrofisica; Italia
Fil: Miceli, M.. Istituto Nazionale di Astrofisica; Italia
Fil: Peres, G.. Istituto Nazionale di Astrofisica; Italia
Fil: Bocchino, F.. Istituto Nazionale di Astrofisica; Italia
Fil: Orlando, S.. Istituto Nazionale di Astrofisica; Italia
Fil: Greco, E.. Istituto Nazionale di Astrofisica; Italia
Fil: Combi, Jorge Ariel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: García, Federico. University Of Groningen. Kapteyn Astronomical Institute; Países Bajos
Fil: Sasaki, M.. Universitat Erlangen-Nuremberg; Alemania
Materia
ISM: INDIVIDUAL OBJECTS: VELA SNR
ISM: SUPERNOVA REMNANTS
X-RAYS: ISM
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:11336/137660
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/137660
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling X-ray emitting structures in the Vela SNR: Ejecta anisotropies and progenitor stellar wind residualsSapienza, V.Miceli, M.Peres, G.Bocchino, F.Orlando, S.Greco, E.Combi, Jorge ArielGarcía, FedericoSasaki, M.ISM: INDIVIDUAL OBJECTS: VELA SNRISM: SUPERNOVA REMNANTSX-RAYS: ISMhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. The Vela supernova remnant (SNR) shows several ejecta fragments (or shrapnel) protruding beyond the forward shock, which are most likely relics of anisotropies that developed during the supernova (SN) explosion. Recent studies have revealed high Si abundance in two shrapnel (shrapnel A and G), located in opposite directions with respect to the SNR center. This suggests the possible existence of a Si-rich jet-counterjet structure, similar to that observed in the SNR Cassiopea A. Aims. We analyzed an XMM-Newton observation of a bright clump, behind shrapnel G, which lies along the direction connecting shrapnel A and G. The aim is to study the physical and chemical properties of this clump to ascertain whether it is part of this putative jet-like structure. Methods. We produced background-corrected and adaptively-smoothed count-rate images and median photon energy maps, and performed a spatially resolved spectral analysis. Results. We identified two structures with different physical properties. The first one is remarkably elongated along the direction connecting shrapnel A and G. Its X-ray spectrum is much softer than that of the other two shrapnel, to the point of hindering the determination of the Si abundance; however, its physical and chemical properties are consistent with those of shrapnel A and shrapnel G. The second structure, running along the southeast-northwest direction, has a higher temperature and appears similar to a thin filament. By analyzing the ROSAT data, we have found that this filament is part of a very large and coherent structure that we identified in the western rim of the shell. Conclusions. We obtained a thorough description of the collimated, jet-like tail of shrapnel G in Vela SNR. In addition we discovered a coherent and very extended feature roughly perpendicular to the jet-like structure that we interpret as a signature of an earlier interaction of the remnant with the stellar wind of its progenitor star. The peculiar Ne/O ratio we found in the wind residual may be suggestive of a Wolf-Rayet progenitor for Vela SNR, though further analysis is required to address this point.Fil: Sapienza, V.. Istituto Nazionale di Astrofisica; ItaliaFil: Miceli, M.. Istituto Nazionale di Astrofisica; ItaliaFil: Peres, G.. Istituto Nazionale di Astrofisica; ItaliaFil: Bocchino, F.. Istituto Nazionale di Astrofisica; ItaliaFil: Orlando, S.. Istituto Nazionale di Astrofisica; ItaliaFil: Greco, E.. Istituto Nazionale di Astrofisica; ItaliaFil: Combi, Jorge Ariel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: García, Federico. University Of Groningen. Kapteyn Astronomical Institute; Países BajosFil: Sasaki, M.. Universitat Erlangen-Nuremberg; AlemaniaEDP Sciences2021-05info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/137660Sapienza, V.; Miceli, M.; Peres, G.; Bocchino, F.; Orlando, S.; et al.; X-ray emitting structures in the Vela SNR: Ejecta anisotropies and progenitor stellar wind residuals; EDP Sciences; Astronomy and Astrophysics; 649; 5-2021; 1-100004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202140412info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2021/05/aa40412-21/aa40412-21.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:12:24Zoai:ri.conicet.gov.ar:11336/137660instacron: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 10:12:24.281CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv X-ray emitting structures in the Vela SNR: Ejecta anisotropies and progenitor stellar wind residuals
title X-ray emitting structures in the Vela SNR: Ejecta anisotropies and progenitor stellar wind residuals
spellingShingle X-ray emitting structures in the Vela SNR: Ejecta anisotropies and progenitor stellar wind residuals
Sapienza, V.
ISM: INDIVIDUAL OBJECTS: VELA SNR
ISM: SUPERNOVA REMNANTS
X-RAYS: ISM
title_short X-ray emitting structures in the Vela SNR: Ejecta anisotropies and progenitor stellar wind residuals
title_full X-ray emitting structures in the Vela SNR: Ejecta anisotropies and progenitor stellar wind residuals
title_fullStr X-ray emitting structures in the Vela SNR: Ejecta anisotropies and progenitor stellar wind residuals
title_full_unstemmed X-ray emitting structures in the Vela SNR: Ejecta anisotropies and progenitor stellar wind residuals
title_sort X-ray emitting structures in the Vela SNR: Ejecta anisotropies and progenitor stellar wind residuals
dc.creator.none.fl_str_mv Sapienza, V.
Miceli, M.
Peres, G.
Bocchino, F.
Orlando, S.
Greco, E.
Combi, Jorge Ariel
García, Federico
Sasaki, M.
author Sapienza, V.
author_facet Sapienza, V.
Miceli, M.
Peres, G.
Bocchino, F.
Orlando, S.
Greco, E.
Combi, Jorge Ariel
García, Federico
Sasaki, M.
author_role author
author2 Miceli, M.
Peres, G.
Bocchino, F.
Orlando, S.
Greco, E.
Combi, Jorge Ariel
García, Federico
Sasaki, M.
author2_role author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv ISM: INDIVIDUAL OBJECTS: VELA SNR
ISM: SUPERNOVA REMNANTS
X-RAYS: ISM
topic ISM: INDIVIDUAL OBJECTS: VELA SNR
ISM: SUPERNOVA REMNANTS
X-RAYS: ISM
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Context. The Vela supernova remnant (SNR) shows several ejecta fragments (or shrapnel) protruding beyond the forward shock, which are most likely relics of anisotropies that developed during the supernova (SN) explosion. Recent studies have revealed high Si abundance in two shrapnel (shrapnel A and G), located in opposite directions with respect to the SNR center. This suggests the possible existence of a Si-rich jet-counterjet structure, similar to that observed in the SNR Cassiopea A. Aims. We analyzed an XMM-Newton observation of a bright clump, behind shrapnel G, which lies along the direction connecting shrapnel A and G. The aim is to study the physical and chemical properties of this clump to ascertain whether it is part of this putative jet-like structure. Methods. We produced background-corrected and adaptively-smoothed count-rate images and median photon energy maps, and performed a spatially resolved spectral analysis. Results. We identified two structures with different physical properties. The first one is remarkably elongated along the direction connecting shrapnel A and G. Its X-ray spectrum is much softer than that of the other two shrapnel, to the point of hindering the determination of the Si abundance; however, its physical and chemical properties are consistent with those of shrapnel A and shrapnel G. The second structure, running along the southeast-northwest direction, has a higher temperature and appears similar to a thin filament. By analyzing the ROSAT data, we have found that this filament is part of a very large and coherent structure that we identified in the western rim of the shell. Conclusions. We obtained a thorough description of the collimated, jet-like tail of shrapnel G in Vela SNR. In addition we discovered a coherent and very extended feature roughly perpendicular to the jet-like structure that we interpret as a signature of an earlier interaction of the remnant with the stellar wind of its progenitor star. The peculiar Ne/O ratio we found in the wind residual may be suggestive of a Wolf-Rayet progenitor for Vela SNR, though further analysis is required to address this point.
Fil: Sapienza, V.. Istituto Nazionale di Astrofisica; Italia
Fil: Miceli, M.. Istituto Nazionale di Astrofisica; Italia
Fil: Peres, G.. Istituto Nazionale di Astrofisica; Italia
Fil: Bocchino, F.. Istituto Nazionale di Astrofisica; Italia
Fil: Orlando, S.. Istituto Nazionale di Astrofisica; Italia
Fil: Greco, E.. Istituto Nazionale di Astrofisica; Italia
Fil: Combi, Jorge Ariel. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: García, Federico. University Of Groningen. Kapteyn Astronomical Institute; Países Bajos
Fil: Sasaki, M.. Universitat Erlangen-Nuremberg; Alemania
description Context. The Vela supernova remnant (SNR) shows several ejecta fragments (or shrapnel) protruding beyond the forward shock, which are most likely relics of anisotropies that developed during the supernova (SN) explosion. Recent studies have revealed high Si abundance in two shrapnel (shrapnel A and G), located in opposite directions with respect to the SNR center. This suggests the possible existence of a Si-rich jet-counterjet structure, similar to that observed in the SNR Cassiopea A. Aims. We analyzed an XMM-Newton observation of a bright clump, behind shrapnel G, which lies along the direction connecting shrapnel A and G. The aim is to study the physical and chemical properties of this clump to ascertain whether it is part of this putative jet-like structure. Methods. We produced background-corrected and adaptively-smoothed count-rate images and median photon energy maps, and performed a spatially resolved spectral analysis. Results. We identified two structures with different physical properties. The first one is remarkably elongated along the direction connecting shrapnel A and G. Its X-ray spectrum is much softer than that of the other two shrapnel, to the point of hindering the determination of the Si abundance; however, its physical and chemical properties are consistent with those of shrapnel A and shrapnel G. The second structure, running along the southeast-northwest direction, has a higher temperature and appears similar to a thin filament. By analyzing the ROSAT data, we have found that this filament is part of a very large and coherent structure that we identified in the western rim of the shell. Conclusions. We obtained a thorough description of the collimated, jet-like tail of shrapnel G in Vela SNR. In addition we discovered a coherent and very extended feature roughly perpendicular to the jet-like structure that we interpret as a signature of an earlier interaction of the remnant with the stellar wind of its progenitor star. The peculiar Ne/O ratio we found in the wind residual may be suggestive of a Wolf-Rayet progenitor for Vela SNR, though further analysis is required to address this point.
publishDate 2021
dc.date.none.fl_str_mv 2021-05
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/11336/137660
Sapienza, V.; Miceli, M.; Peres, G.; Bocchino, F.; Orlando, S.; et al.; X-ray emitting structures in the Vela SNR: Ejecta anisotropies and progenitor stellar wind residuals; EDP Sciences; Astronomy and Astrophysics; 649; 5-2021; 1-10
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/137660
identifier_str_mv Sapienza, V.; Miceli, M.; Peres, G.; Bocchino, F.; Orlando, S.; et al.; X-ray emitting structures in the Vela SNR: Ejecta anisotropies and progenitor stellar wind residuals; EDP Sciences; Astronomy and Astrophysics; 649; 5-2021; 1-10
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/10.1051/0004-6361/202140412
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2021/05/aa40412-21/aa40412-21.html
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 13.070432

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