A joint spectro-imaging analysis of the XMM-Newton and HESS observations of the supernova remnant RX J1713.7-3946

Autores
Acero Barriga, Fabio Nelson; Ballet, J.; Decourchelle, A.; Lemoine Goumard, M.; Ortega, Martin Eduardo; Giacani, Elsa Beatriz; Dubner, Gloria Mabel; Cassam Chenai, G.
Año de publicación
2008
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. The supernova remnant (SNR) RX J1713.7-3946 (also known as G347.3-0.5) is part of the class of remnants dominated by synchrotron emission in X-rays. It is also one of the few shell-type SNRs observed at TeV energies allowing to investigate particle acceleration at SNRs shock. Aims. Our goal is to compare spatial and spectral properties of the remnant in X- and  -rays to understand the nature of the TeV emission. This requires to study the remnant at the same spatial scale at both energies. To complement the non-thermal spectrum of the remnant, we attempt to provide a reliable estimate for the radio flux density. Methods. In radio, we revisited ATCA data and used HI and mid-infrared observations to disentangle the thermal from the nonthermal emission. In X-rays, we produced a new mosaic of the remnant and degraded the spatial resolution of the X-ray data to the resolution of the HESS instrument to perform spatially resolved spectroscopy at the same spatial scale in X- and  gamma-rays. Radial profiles were obtained to investigate the extension of the emission at both energies. Results. We found that part of the radio emission within the SNR contours is thermal in nature. Taking this into account, we provide new lower and upper limits for the integrated synchrotron flux of the remnant at 1.4 GHz of 22 Jy and 26 Jy respectively. In X-rays, we obtained the first full coverage of RX J1713.7-3946 with XMM-Newton. The spatial variation of the photon index seen at small scale in X-rays is smeared out at HESS resolution. A non-linear correlation between the X- and  gamma-ray fluxes of the type F_X propto F_gamma^2.41   is found. If the flux variation are mainly due to density variation around the remnant then a leptonic model can more easily reproduce the observed X/ -ray correlation. In some angular sectors, radial profiles indicate that the bulk of the X-ray emission comes more from the inside of the remnant than in  gamma-rays.
Fil: Acero Barriga, Fabio Nelson. Université Paris Diderot - Paris 7; Francia
Fil: Ballet, J.. Université Paris Diderot - Paris 7; Francia
Fil: Decourchelle, A.. Université Paris Diderot - Paris 7; Francia
Fil: Lemoine Goumard, M.. Centre d’Etudes nucleaires de Bordeaux Gradignan; Francia
Fil: Ortega, Martin Eduardo. 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: Giacani, Elsa Beatriz. 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: Dubner, Gloria Mabel. 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: Cassam Chenai, G.. Osservatorio Astrofisico di Arcetri; Italia
Materia
ACCELERATION OF PARTICLES
ISM: SUPERNOVA REMNANTS
RADIATION MECHANISMS: NON-THERMAL
X-RAYS: INDIVIDUALS: RX J1713.7-3946
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:11336/20713
Acceder
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network_name_str CONICET Digital (CONICET)
spelling A joint spectro-imaging analysis of the XMM-Newton and HESS observations of the supernova remnant RX J1713.7-3946Acero Barriga, Fabio NelsonBallet, J.Decourchelle, A.Lemoine Goumard, M.Ortega, Martin EduardoGiacani, Elsa BeatrizDubner, Gloria MabelCassam Chenai, G.ACCELERATION OF PARTICLESISM: SUPERNOVA REMNANTSRADIATION MECHANISMS: NON-THERMALX-RAYS: INDIVIDUALS: RX J1713.7-3946https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. The supernova remnant (SNR) RX J1713.7-3946 (also known as G347.3-0.5) is part of the class of remnants dominated by synchrotron emission in X-rays. It is also one of the few shell-type SNRs observed at TeV energies allowing to investigate particle acceleration at SNRs shock. Aims. Our goal is to compare spatial and spectral properties of the remnant in X- and  -rays to understand the nature of the TeV emission. This requires to study the remnant at the same spatial scale at both energies. To complement the non-thermal spectrum of the remnant, we attempt to provide a reliable estimate for the radio flux density. Methods. In radio, we revisited ATCA data and used HI and mid-infrared observations to disentangle the thermal from the nonthermal emission. In X-rays, we produced a new mosaic of the remnant and degraded the spatial resolution of the X-ray data to the resolution of the HESS instrument to perform spatially resolved spectroscopy at the same spatial scale in X- and  gamma-rays. Radial profiles were obtained to investigate the extension of the emission at both energies. Results. We found that part of the radio emission within the SNR contours is thermal in nature. Taking this into account, we provide new lower and upper limits for the integrated synchrotron flux of the remnant at 1.4 GHz of 22 Jy and 26 Jy respectively. In X-rays, we obtained the first full coverage of RX J1713.7-3946 with XMM-Newton. The spatial variation of the photon index seen at small scale in X-rays is smeared out at HESS resolution. A non-linear correlation between the X- and  gamma-ray fluxes of the type F_X propto F_gamma^2.41   is found. If the flux variation are mainly due to density variation around the remnant then a leptonic model can more easily reproduce the observed X/ -ray correlation. In some angular sectors, radial profiles indicate that the bulk of the X-ray emission comes more from the inside of the remnant than in  gamma-rays.Fil: Acero Barriga, Fabio Nelson. Université Paris Diderot - Paris 7; FranciaFil: Ballet, J.. Université Paris Diderot - Paris 7; FranciaFil: Decourchelle, A.. Université Paris Diderot - Paris 7; FranciaFil: Lemoine Goumard, M.. Centre d’Etudes nucleaires de Bordeaux Gradignan; FranciaFil: Ortega, Martin Eduardo. 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: Giacani, Elsa Beatriz. 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: Dubner, Gloria Mabel. 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: Cassam Chenai, G.. Osservatorio Astrofisico di Arcetri; ItaliaEDP Sciences2008-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/20713Acero Barriga, Fabio Nelson; Ballet, J.; Decourchelle, A.; Lemoine Goumard, M.; Ortega, Martin Eduardo; et al.; A joint spectro-imaging analysis of the XMM-Newton and HESS observations of the supernova remnant RX J1713.7-3946; EDP Sciences; Astronomy and Astrophysics; 505; 1; 12-2008; 157-1670004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2009/37/aa11556-08/aa11556-08.htmlinfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/200811556info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/0906.1073info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:42:29Zoai:ri.conicet.gov.ar:11336/20713instacron: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 09:42:29.357CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv A joint spectro-imaging analysis of the XMM-Newton and HESS observations of the supernova remnant RX J1713.7-3946
title A joint spectro-imaging analysis of the XMM-Newton and HESS observations of the supernova remnant RX J1713.7-3946
spellingShingle A joint spectro-imaging analysis of the XMM-Newton and HESS observations of the supernova remnant RX J1713.7-3946
Acero Barriga, Fabio Nelson
ACCELERATION OF PARTICLES
ISM: SUPERNOVA REMNANTS
RADIATION MECHANISMS: NON-THERMAL
X-RAYS: INDIVIDUALS: RX J1713.7-3946
title_short A joint spectro-imaging analysis of the XMM-Newton and HESS observations of the supernova remnant RX J1713.7-3946
title_full A joint spectro-imaging analysis of the XMM-Newton and HESS observations of the supernova remnant RX J1713.7-3946
title_fullStr A joint spectro-imaging analysis of the XMM-Newton and HESS observations of the supernova remnant RX J1713.7-3946
title_full_unstemmed A joint spectro-imaging analysis of the XMM-Newton and HESS observations of the supernova remnant RX J1713.7-3946
title_sort A joint spectro-imaging analysis of the XMM-Newton and HESS observations of the supernova remnant RX J1713.7-3946
dc.creator.none.fl_str_mv Acero Barriga, Fabio Nelson
Ballet, J.
Decourchelle, A.
Lemoine Goumard, M.
Ortega, Martin Eduardo
Giacani, Elsa Beatriz
Dubner, Gloria Mabel
Cassam Chenai, G.
author Acero Barriga, Fabio Nelson
author_facet Acero Barriga, Fabio Nelson
Ballet, J.
Decourchelle, A.
Lemoine Goumard, M.
Ortega, Martin Eduardo
Giacani, Elsa Beatriz
Dubner, Gloria Mabel
Cassam Chenai, G.
author_role author
author2 Ballet, J.
Decourchelle, A.
Lemoine Goumard, M.
Ortega, Martin Eduardo
Giacani, Elsa Beatriz
Dubner, Gloria Mabel
Cassam Chenai, G.
author2_role author
author
author
author
author
author
author
dc.subject.none.fl_str_mv ACCELERATION OF PARTICLES
ISM: SUPERNOVA REMNANTS
RADIATION MECHANISMS: NON-THERMAL
X-RAYS: INDIVIDUALS: RX J1713.7-3946
topic ACCELERATION OF PARTICLES
ISM: SUPERNOVA REMNANTS
RADIATION MECHANISMS: NON-THERMAL
X-RAYS: INDIVIDUALS: RX J1713.7-3946
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 supernova remnant (SNR) RX J1713.7-3946 (also known as G347.3-0.5) is part of the class of remnants dominated by synchrotron emission in X-rays. It is also one of the few shell-type SNRs observed at TeV energies allowing to investigate particle acceleration at SNRs shock. Aims. Our goal is to compare spatial and spectral properties of the remnant in X- and  -rays to understand the nature of the TeV emission. This requires to study the remnant at the same spatial scale at both energies. To complement the non-thermal spectrum of the remnant, we attempt to provide a reliable estimate for the radio flux density. Methods. In radio, we revisited ATCA data and used HI and mid-infrared observations to disentangle the thermal from the nonthermal emission. In X-rays, we produced a new mosaic of the remnant and degraded the spatial resolution of the X-ray data to the resolution of the HESS instrument to perform spatially resolved spectroscopy at the same spatial scale in X- and  gamma-rays. Radial profiles were obtained to investigate the extension of the emission at both energies. Results. We found that part of the radio emission within the SNR contours is thermal in nature. Taking this into account, we provide new lower and upper limits for the integrated synchrotron flux of the remnant at 1.4 GHz of 22 Jy and 26 Jy respectively. In X-rays, we obtained the first full coverage of RX J1713.7-3946 with XMM-Newton. The spatial variation of the photon index seen at small scale in X-rays is smeared out at HESS resolution. A non-linear correlation between the X- and  gamma-ray fluxes of the type F_X propto F_gamma^2.41   is found. If the flux variation are mainly due to density variation around the remnant then a leptonic model can more easily reproduce the observed X/ -ray correlation. In some angular sectors, radial profiles indicate that the bulk of the X-ray emission comes more from the inside of the remnant than in  gamma-rays.
Fil: Acero Barriga, Fabio Nelson. Université Paris Diderot - Paris 7; Francia
Fil: Ballet, J.. Université Paris Diderot - Paris 7; Francia
Fil: Decourchelle, A.. Université Paris Diderot - Paris 7; Francia
Fil: Lemoine Goumard, M.. Centre d’Etudes nucleaires de Bordeaux Gradignan; Francia
Fil: Ortega, Martin Eduardo. 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: Giacani, Elsa Beatriz. 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: Dubner, Gloria Mabel. 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: Cassam Chenai, G.. Osservatorio Astrofisico di Arcetri; Italia
description Context. The supernova remnant (SNR) RX J1713.7-3946 (also known as G347.3-0.5) is part of the class of remnants dominated by synchrotron emission in X-rays. It is also one of the few shell-type SNRs observed at TeV energies allowing to investigate particle acceleration at SNRs shock. Aims. Our goal is to compare spatial and spectral properties of the remnant in X- and  -rays to understand the nature of the TeV emission. This requires to study the remnant at the same spatial scale at both energies. To complement the non-thermal spectrum of the remnant, we attempt to provide a reliable estimate for the radio flux density. Methods. In radio, we revisited ATCA data and used HI and mid-infrared observations to disentangle the thermal from the nonthermal emission. In X-rays, we produced a new mosaic of the remnant and degraded the spatial resolution of the X-ray data to the resolution of the HESS instrument to perform spatially resolved spectroscopy at the same spatial scale in X- and  gamma-rays. Radial profiles were obtained to investigate the extension of the emission at both energies. Results. We found that part of the radio emission within the SNR contours is thermal in nature. Taking this into account, we provide new lower and upper limits for the integrated synchrotron flux of the remnant at 1.4 GHz of 22 Jy and 26 Jy respectively. In X-rays, we obtained the first full coverage of RX J1713.7-3946 with XMM-Newton. The spatial variation of the photon index seen at small scale in X-rays is smeared out at HESS resolution. A non-linear correlation between the X- and  gamma-ray fluxes of the type F_X propto F_gamma^2.41   is found. If the flux variation are mainly due to density variation around the remnant then a leptonic model can more easily reproduce the observed X/ -ray correlation. In some angular sectors, radial profiles indicate that the bulk of the X-ray emission comes more from the inside of the remnant than in  gamma-rays.
publishDate 2008
dc.date.none.fl_str_mv 2008-12
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/11336/20713
Acero Barriga, Fabio Nelson; Ballet, J.; Decourchelle, A.; Lemoine Goumard, M.; Ortega, Martin Eduardo; et al.; A joint spectro-imaging analysis of the XMM-Newton and HESS observations of the supernova remnant RX J1713.7-3946; EDP Sciences; Astronomy and Astrophysics; 505; 1; 12-2008; 157-167
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/20713
identifier_str_mv Acero Barriga, Fabio Nelson; Ballet, J.; Decourchelle, A.; Lemoine Goumard, M.; Ortega, Martin Eduardo; et al.; A joint spectro-imaging analysis of the XMM-Newton and HESS observations of the supernova remnant RX J1713.7-3946; EDP Sciences; Astronomy and Astrophysics; 505; 1; 12-2008; 157-167
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/url/https://www.aanda.org/articles/aa/full_html/2009/37/aa11556-08/aa11556-08.html
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/200811556
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/0906.1073
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)
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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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