XMM-Newton detection of the supernova remnant G304.6+0.1 (Kes 17)

Autores
Combi, Jorge Ariel; Albacete Colombo, Juan Facundo; Sánchez Ayaso, Estrella; Romero, Gustavo Esteban; Marti, J.; Luque Escamilla, P. L.; Muñoz Arjonilla, A. J.; Sánchez Sutil, J. R.; López Santiago, J.
Año de publicación
2010
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Aims. We report the first detailed X-ray study of the supernova remnant (SNR) G304.6+0.1, achieved with the XMM-Newton mission. Methods. The powerful imaging capability of XMM-Newton was used to study the X-ray characteristics of the remnant at different energy ranges. The X-ray morphology and spectral properties were analyzed. In addittion, radio and mid-infrared data obtained with the Molonglo Observatory Synthesis Telescope and the Spitzer Space Telescope were used to study the association with the detected X-ray emission and to understand the structure of the SNR at differents wavelengths. Results. The SNR shows an extended and arc-like internal structure in the X-ray band without a compact point-like source inside the remnant. We find a high column density of NH in the range 2.5–3.5 × 1022 cm−2, which supports a relatively distant location (d ≥ 9.7 kpc). The X-ray spectrum exhibits at least three emission lines, indicating that the X-ray emission has a thin thermal plasma origin, although a non-thermal contribution cannot be discarded. The spectra of three different regions (north, center and south) are well represented by a combination of a non-equilibrium ionization (PSHOCK) and a power-law (PL) model. The mid-infrared observations show a bright filamentary structure along the north-south direction coincident with the NW radio shell. This suggests that Kes 17 is propagating in a non-uniform environment with high density and that the shock front is interacting with several adjacent massive molecular clouds. The good correspondence of radio and mid-infrared emissions suggests that the filamentary features are caused by shock compression. The X-ray characteristics and well-known radio parameters indicate that G304.6+0.1 is a middle-aged SNR (2.8−6.4) × 104 yr old and a new member of the recently proposed group of mixed-morphology SNRs.
Fil: Combi, Jorge Ariel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto Argentino de Radioastronomia (i); Argentina. Universidad de Jaén; España. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Albacete Colombo, Juan Facundo. Universidad Nacional del Comahue; Argentina
Fil: Sánchez Ayaso, Estrella. Universidad de Jaén; España
Fil: Romero, Gustavo Esteban. 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: Marti, J.. Universidad de Jaén; España
Fil: Luque Escamilla, P. L.. Escuela Politécnica Superior, Universidad de Jaén. Departamento de Ingeniería Mecánica y Minera; España
Fil: Muñoz Arjonilla, A. J.. Escuela Politécnica Superior, Universidad de Jaén. Departamento de Ingeniería Mecánica y Minera; España
Fil: Sánchez Sutil, J. R.. Escuela Politécnica Superior, Universidad de Jaén. Departamento de Ingeniería Mecánica y Minera; España
Fil: López Santiago, J.. Universidad Complutense de Madrid. Departamento de Astrofísica y Ciencias de la Atmósfera; España
Materia
ISM: individual objects: G304.6+0.1
ISM: supernova remnants
X-rays: ISM
Radiation mechanisms: 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:11336/18905
Acceder
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network_name_str CONICET Digital (CONICET)
spelling XMM-Newton detection of the supernova remnant G304.6+0.1 (Kes 17)Combi, Jorge ArielAlbacete Colombo, Juan FacundoSánchez Ayaso, EstrellaRomero, Gustavo EstebanMarti, J.Luque Escamilla, P. L.Muñoz Arjonilla, A. J.Sánchez Sutil, J. R.López Santiago, J.ISM: individual objects: G304.6+0.1ISM: supernova remnantsX-rays: ISMRadiation mechanisms: thermalhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Aims. We report the first detailed X-ray study of the supernova remnant (SNR) G304.6+0.1, achieved with the XMM-Newton mission. Methods. The powerful imaging capability of XMM-Newton was used to study the X-ray characteristics of the remnant at different energy ranges. The X-ray morphology and spectral properties were analyzed. In addittion, radio and mid-infrared data obtained with the Molonglo Observatory Synthesis Telescope and the Spitzer Space Telescope were used to study the association with the detected X-ray emission and to understand the structure of the SNR at differents wavelengths. Results. The SNR shows an extended and arc-like internal structure in the X-ray band without a compact point-like source inside the remnant. We find a high column density of NH in the range 2.5–3.5 × 1022 cm−2, which supports a relatively distant location (d ≥ 9.7 kpc). The X-ray spectrum exhibits at least three emission lines, indicating that the X-ray emission has a thin thermal plasma origin, although a non-thermal contribution cannot be discarded. The spectra of three different regions (north, center and south) are well represented by a combination of a non-equilibrium ionization (PSHOCK) and a power-law (PL) model. The mid-infrared observations show a bright filamentary structure along the north-south direction coincident with the NW radio shell. This suggests that Kes 17 is propagating in a non-uniform environment with high density and that the shock front is interacting with several adjacent massive molecular clouds. The good correspondence of radio and mid-infrared emissions suggests that the filamentary features are caused by shock compression. The X-ray characteristics and well-known radio parameters indicate that G304.6+0.1 is a middle-aged SNR (2.8−6.4) × 104 yr old and a new member of the recently proposed group of mixed-morphology SNRs.Fil: Combi, Jorge Ariel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto Argentino de Radioastronomia (i); Argentina. Universidad de Jaén; España. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Albacete Colombo, Juan Facundo. Universidad Nacional del Comahue; ArgentinaFil: Sánchez Ayaso, Estrella. Universidad de Jaén; EspañaFil: Romero, Gustavo Esteban. 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: Marti, J.. Universidad de Jaén; EspañaFil: Luque Escamilla, P. L.. Escuela Politécnica Superior, Universidad de Jaén. Departamento de Ingeniería Mecánica y Minera; EspañaFil: Muñoz Arjonilla, A. J.. Escuela Politécnica Superior, Universidad de Jaén. Departamento de Ingeniería Mecánica y Minera; EspañaFil: Sánchez Sutil, J. R.. Escuela Politécnica Superior, Universidad de Jaén. Departamento de Ingeniería Mecánica y Minera; EspañaFil: López Santiago, J.. Universidad Complutense de Madrid. Departamento de Astrofísica y Ciencias de la Atmósfera; EspañaEdp Sciences2010-09-13info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/18905Combi, Jorge Ariel; Albacete Colombo, Juan Facundo; Sánchez Ayaso, Estrella; Romero, Gustavo Esteban; Marti, J.; et al.; XMM-Newton detection of the supernova remnant G304.6+0.1 (Kes 17); Edp Sciences; Astronomy And Astrophysics; 523; 13-9-2010; 76-800004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010A%26A...523A..76C&db_key=AST&link_type=ABSTRACT&high=4cf3bad8a512265info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/200913935info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2010/15/aa13935-09/aa13935-09.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 Técnicas2025-09-03T10:07:24Zoai:ri.conicet.gov.ar:11336/18905instacron: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:34982025-09-03 10:07:24.801CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv XMM-Newton detection of the supernova remnant G304.6+0.1 (Kes 17)
title XMM-Newton detection of the supernova remnant G304.6+0.1 (Kes 17)
spellingShingle XMM-Newton detection of the supernova remnant G304.6+0.1 (Kes 17)
Combi, Jorge Ariel
ISM: individual objects: G304.6+0.1
ISM: supernova remnants
X-rays: ISM
Radiation mechanisms: thermal
title_short XMM-Newton detection of the supernova remnant G304.6+0.1 (Kes 17)
title_full XMM-Newton detection of the supernova remnant G304.6+0.1 (Kes 17)
title_fullStr XMM-Newton detection of the supernova remnant G304.6+0.1 (Kes 17)
title_full_unstemmed XMM-Newton detection of the supernova remnant G304.6+0.1 (Kes 17)
title_sort XMM-Newton detection of the supernova remnant G304.6+0.1 (Kes 17)
dc.creator.none.fl_str_mv Combi, Jorge Ariel
Albacete Colombo, Juan Facundo
Sánchez Ayaso, Estrella
Romero, Gustavo Esteban
Marti, J.
Luque Escamilla, P. L.
Muñoz Arjonilla, A. J.
Sánchez Sutil, J. R.
López Santiago, J.
author Combi, Jorge Ariel
author_facet Combi, Jorge Ariel
Albacete Colombo, Juan Facundo
Sánchez Ayaso, Estrella
Romero, Gustavo Esteban
Marti, J.
Luque Escamilla, P. L.
Muñoz Arjonilla, A. J.
Sánchez Sutil, J. R.
López Santiago, J.
author_role author
author2 Albacete Colombo, Juan Facundo
Sánchez Ayaso, Estrella
Romero, Gustavo Esteban
Marti, J.
Luque Escamilla, P. L.
Muñoz Arjonilla, A. J.
Sánchez Sutil, J. R.
López Santiago, J.
author2_role author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv ISM: individual objects: G304.6+0.1
ISM: supernova remnants
X-rays: ISM
Radiation mechanisms: thermal
topic ISM: individual objects: G304.6+0.1
ISM: supernova remnants
X-rays: ISM
Radiation mechanisms: 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 report the first detailed X-ray study of the supernova remnant (SNR) G304.6+0.1, achieved with the XMM-Newton mission. Methods. The powerful imaging capability of XMM-Newton was used to study the X-ray characteristics of the remnant at different energy ranges. The X-ray morphology and spectral properties were analyzed. In addittion, radio and mid-infrared data obtained with the Molonglo Observatory Synthesis Telescope and the Spitzer Space Telescope were used to study the association with the detected X-ray emission and to understand the structure of the SNR at differents wavelengths. Results. The SNR shows an extended and arc-like internal structure in the X-ray band without a compact point-like source inside the remnant. We find a high column density of NH in the range 2.5–3.5 × 1022 cm−2, which supports a relatively distant location (d ≥ 9.7 kpc). The X-ray spectrum exhibits at least three emission lines, indicating that the X-ray emission has a thin thermal plasma origin, although a non-thermal contribution cannot be discarded. The spectra of three different regions (north, center and south) are well represented by a combination of a non-equilibrium ionization (PSHOCK) and a power-law (PL) model. The mid-infrared observations show a bright filamentary structure along the north-south direction coincident with the NW radio shell. This suggests that Kes 17 is propagating in a non-uniform environment with high density and that the shock front is interacting with several adjacent massive molecular clouds. The good correspondence of radio and mid-infrared emissions suggests that the filamentary features are caused by shock compression. The X-ray characteristics and well-known radio parameters indicate that G304.6+0.1 is a middle-aged SNR (2.8−6.4) × 104 yr old and a new member of the recently proposed group of mixed-morphology SNRs.
Fil: Combi, Jorge Ariel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto Argentino de Radioastronomia (i); Argentina. Universidad de Jaén; España. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Fil: Albacete Colombo, Juan Facundo. Universidad Nacional del Comahue; Argentina
Fil: Sánchez Ayaso, Estrella. Universidad de Jaén; España
Fil: Romero, Gustavo Esteban. 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: Marti, J.. Universidad de Jaén; España
Fil: Luque Escamilla, P. L.. Escuela Politécnica Superior, Universidad de Jaén. Departamento de Ingeniería Mecánica y Minera; España
Fil: Muñoz Arjonilla, A. J.. Escuela Politécnica Superior, Universidad de Jaén. Departamento de Ingeniería Mecánica y Minera; España
Fil: Sánchez Sutil, J. R.. Escuela Politécnica Superior, Universidad de Jaén. Departamento de Ingeniería Mecánica y Minera; España
Fil: López Santiago, J.. Universidad Complutense de Madrid. Departamento de Astrofísica y Ciencias de la Atmósfera; España
description Aims. We report the first detailed X-ray study of the supernova remnant (SNR) G304.6+0.1, achieved with the XMM-Newton mission. Methods. The powerful imaging capability of XMM-Newton was used to study the X-ray characteristics of the remnant at different energy ranges. The X-ray morphology and spectral properties were analyzed. In addittion, radio and mid-infrared data obtained with the Molonglo Observatory Synthesis Telescope and the Spitzer Space Telescope were used to study the association with the detected X-ray emission and to understand the structure of the SNR at differents wavelengths. Results. The SNR shows an extended and arc-like internal structure in the X-ray band without a compact point-like source inside the remnant. We find a high column density of NH in the range 2.5–3.5 × 1022 cm−2, which supports a relatively distant location (d ≥ 9.7 kpc). The X-ray spectrum exhibits at least three emission lines, indicating that the X-ray emission has a thin thermal plasma origin, although a non-thermal contribution cannot be discarded. The spectra of three different regions (north, center and south) are well represented by a combination of a non-equilibrium ionization (PSHOCK) and a power-law (PL) model. The mid-infrared observations show a bright filamentary structure along the north-south direction coincident with the NW radio shell. This suggests that Kes 17 is propagating in a non-uniform environment with high density and that the shock front is interacting with several adjacent massive molecular clouds. The good correspondence of radio and mid-infrared emissions suggests that the filamentary features are caused by shock compression. The X-ray characteristics and well-known radio parameters indicate that G304.6+0.1 is a middle-aged SNR (2.8−6.4) × 104 yr old and a new member of the recently proposed group of mixed-morphology SNRs.
publishDate 2010
dc.date.none.fl_str_mv 2010-09-13
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/11336/18905
Combi, Jorge Ariel; Albacete Colombo, Juan Facundo; Sánchez Ayaso, Estrella; Romero, Gustavo Esteban; Marti, J.; et al.; XMM-Newton detection of the supernova remnant G304.6+0.1 (Kes 17); Edp Sciences; Astronomy And Astrophysics; 523; 13-9-2010; 76-80
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/18905
identifier_str_mv Combi, Jorge Ariel; Albacete Colombo, Juan Facundo; Sánchez Ayaso, Estrella; Romero, Gustavo Esteban; Marti, J.; et al.; XMM-Newton detection of the supernova remnant G304.6+0.1 (Kes 17); Edp Sciences; Astronomy And Astrophysics; 523; 13-9-2010; 76-80
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/http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010A%26A...523A..76C&db_key=AST&link_type=ABSTRACT&high=4cf3bad8a512265
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/200913935
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2010/15/aa13935-09/aa13935-09.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 13.13397

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