The interaction of SNR Kes 17 with the interstellar medium: Fresh view from radio and γ-rays

Autores
Supán, Jorge Leonardo; Castelletti, Gabriela Marta; Lemiere, A.
Año de publicación
2023
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
This paper presents a comprehensive analysis of the Galactic supernova remnant (SNR) Kes 17 (G304.6+0.1) with a focus on its radio synchrotron emission, environs, and the factors contributing to the observed gamma rays. The fitting to the firstly-obtained integrated radio continuum spectrum spanning from 88 to 8800 MHz yields an index alpha = -0.488 +/- 0.023 (S propto nu^alpha), indicative of a linear particle acceleration process at the shock front of the remnant. Accounting for the SNR radio shell size, the distribution of atomic hydrogen (nH ~ 10 cm-3), and assuming the SNR is in the Sedov-Taylor stage of its evolution, we estimate the remnant’s age to be roughly 8.5 kyr. This result falls at the lower end of the wide range (~2-64 kyr) derived from previous analyses of the diffuse X-ray emission interior to the remnant. Furthermore, we used 12CO and 13CO (J=1-0) emission-line data as a proxy for molecular hydrogen and provided the first evidence that the eastern shell of Kes 17 is engulfing a molecular enhancement in the surrounding gas, with an average mass 4.2 x 10^4 Msun and density n ~ 300 cm-3. Towards the western boundary of Kes 17 there are not signatures of carbon monoxide emissions above 3sigma, despite previously reported infrared observations have revealed shocked molecular gas at that location. This suggests the existence of a CO-dark interacting molecular gas, a phenomenon also recorded in other Galactic SNRs (e.g. CTB 37A and RX J1713.7-3946) brightening both in the infrared and gamma-ray domains. Additionally, by analysing ~14.5 yr of continuously collected data from the Large Area Telescope on board the satellite Fermi, we determined that the best-fit power-law photon index for the 0.3-300 GeV gamma-ray emission from the Kes 17 region is Gamma = 2.39 +/- 0.04 +0.063 -0.114 (+/-stat +/-syst) in agreement with prior studies. The energy flux turns out to be (2.98 +/- 0.14) x 10^-11 erg cm-2 s-1 implying a luminosity (2.22 +/- 0.45) x 10^35 erg s-1 at ~ 8 kpc. Finally, we successfully modelled the multiwavelength spectral energy distribution by incorporating the radio synchrotron spectrum and the new measurements of GeV gamma-rays. Our analysis indicates that the observed gamma-ray flux most likely originates from the interaction of Kes 17 with western "dark" CO zone with a proton density np ~400 cm-3.
Fil: Supán, Jorge Leonardo. Consejo Nacional de Investigaciones 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: Castelletti, Gabriela Marta. Consejo Nacional de Investigaciones 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: Lemiere, A.. Centre National de la Recherche Scientifique; Francia
Materia
ISM: SUPERNOVA REMNANTS
ISM: INDIVIDUAL OBJECTS: KES 17
RADIO CONTINUUM: GENERAL
GAMMA 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:11336/235586

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network_name_str CONICET Digital (CONICET)
spelling The interaction of SNR Kes 17 with the interstellar medium: Fresh view from radio and γ-raysSupán, Jorge LeonardoCastelletti, Gabriela MartaLemiere, A.ISM: SUPERNOVA REMNANTSISM: INDIVIDUAL OBJECTS: KES 17RADIO CONTINUUM: GENERALGAMMA RAYS: ISMhttps://purl.org/becyt/ford/1.7https://purl.org/becyt/ford/1This paper presents a comprehensive analysis of the Galactic supernova remnant (SNR) Kes 17 (G304.6+0.1) with a focus on its radio synchrotron emission, environs, and the factors contributing to the observed gamma rays. The fitting to the firstly-obtained integrated radio continuum spectrum spanning from 88 to 8800 MHz yields an index alpha = -0.488 +/- 0.023 (S propto nu^alpha), indicative of a linear particle acceleration process at the shock front of the remnant. Accounting for the SNR radio shell size, the distribution of atomic hydrogen (nH ~ 10 cm-3), and assuming the SNR is in the Sedov-Taylor stage of its evolution, we estimate the remnant’s age to be roughly 8.5 kyr. This result falls at the lower end of the wide range (~2-64 kyr) derived from previous analyses of the diffuse X-ray emission interior to the remnant. Furthermore, we used 12CO and 13CO (J=1-0) emission-line data as a proxy for molecular hydrogen and provided the first evidence that the eastern shell of Kes 17 is engulfing a molecular enhancement in the surrounding gas, with an average mass 4.2 x 10^4 Msun and density n ~ 300 cm-3. Towards the western boundary of Kes 17 there are not signatures of carbon monoxide emissions above 3sigma, despite previously reported infrared observations have revealed shocked molecular gas at that location. This suggests the existence of a CO-dark interacting molecular gas, a phenomenon also recorded in other Galactic SNRs (e.g. CTB 37A and RX J1713.7-3946) brightening both in the infrared and gamma-ray domains. Additionally, by analysing ~14.5 yr of continuously collected data from the Large Area Telescope on board the satellite Fermi, we determined that the best-fit power-law photon index for the 0.3-300 GeV gamma-ray emission from the Kes 17 region is Gamma = 2.39 +/- 0.04 +0.063 -0.114 (+/-stat +/-syst) in agreement with prior studies. The energy flux turns out to be (2.98 +/- 0.14) x 10^-11 erg cm-2 s-1 implying a luminosity (2.22 +/- 0.45) x 10^35 erg s-1 at ~ 8 kpc. Finally, we successfully modelled the multiwavelength spectral energy distribution by incorporating the radio synchrotron spectrum and the new measurements of GeV gamma-rays. Our analysis indicates that the observed gamma-ray flux most likely originates from the interaction of Kes 17 with western "dark" CO zone with a proton density np ~400 cm-3.Fil: Supán, Jorge Leonardo. Consejo Nacional de Investigaciones 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: Castelletti, Gabriela Marta. Consejo Nacional de Investigaciones 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: Lemiere, A.. Centre National de la Recherche Scientifique; FranciaEDP Sciences2023-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/235586Supán, Jorge Leonardo; Castelletti, Gabriela Marta; Lemiere, A.; The interaction of SNR Kes 17 with the interstellar medium: Fresh view from radio and γ-rays; EDP Sciences; Astronomy and Astrophysics; 679; 7-2023; 1-101432-0746CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/pdf/2023/11/aa47305-23.pdfinfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202347305info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:01:57Zoai:ri.conicet.gov.ar:11336/235586instacron: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 10:01:57.864CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The interaction of SNR Kes 17 with the interstellar medium: Fresh view from radio and γ-rays
title The interaction of SNR Kes 17 with the interstellar medium: Fresh view from radio and γ-rays
spellingShingle The interaction of SNR Kes 17 with the interstellar medium: Fresh view from radio and γ-rays
Supán, Jorge Leonardo
ISM: SUPERNOVA REMNANTS
ISM: INDIVIDUAL OBJECTS: KES 17
RADIO CONTINUUM: GENERAL
GAMMA RAYS: ISM
title_short The interaction of SNR Kes 17 with the interstellar medium: Fresh view from radio and γ-rays
title_full The interaction of SNR Kes 17 with the interstellar medium: Fresh view from radio and γ-rays
title_fullStr The interaction of SNR Kes 17 with the interstellar medium: Fresh view from radio and γ-rays
title_full_unstemmed The interaction of SNR Kes 17 with the interstellar medium: Fresh view from radio and γ-rays
title_sort The interaction of SNR Kes 17 with the interstellar medium: Fresh view from radio and γ-rays
dc.creator.none.fl_str_mv Supán, Jorge Leonardo
Castelletti, Gabriela Marta
Lemiere, A.
author Supán, Jorge Leonardo
author_facet Supán, Jorge Leonardo
Castelletti, Gabriela Marta
Lemiere, A.
author_role author
author2 Castelletti, Gabriela Marta
Lemiere, A.
author2_role author
author
dc.subject.none.fl_str_mv ISM: SUPERNOVA REMNANTS
ISM: INDIVIDUAL OBJECTS: KES 17
RADIO CONTINUUM: GENERAL
GAMMA RAYS: ISM
topic ISM: SUPERNOVA REMNANTS
ISM: INDIVIDUAL OBJECTS: KES 17
RADIO CONTINUUM: GENERAL
GAMMA RAYS: ISM
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.7
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv This paper presents a comprehensive analysis of the Galactic supernova remnant (SNR) Kes 17 (G304.6+0.1) with a focus on its radio synchrotron emission, environs, and the factors contributing to the observed gamma rays. The fitting to the firstly-obtained integrated radio continuum spectrum spanning from 88 to 8800 MHz yields an index alpha = -0.488 +/- 0.023 (S propto nu^alpha), indicative of a linear particle acceleration process at the shock front of the remnant. Accounting for the SNR radio shell size, the distribution of atomic hydrogen (nH ~ 10 cm-3), and assuming the SNR is in the Sedov-Taylor stage of its evolution, we estimate the remnant’s age to be roughly 8.5 kyr. This result falls at the lower end of the wide range (~2-64 kyr) derived from previous analyses of the diffuse X-ray emission interior to the remnant. Furthermore, we used 12CO and 13CO (J=1-0) emission-line data as a proxy for molecular hydrogen and provided the first evidence that the eastern shell of Kes 17 is engulfing a molecular enhancement in the surrounding gas, with an average mass 4.2 x 10^4 Msun and density n ~ 300 cm-3. Towards the western boundary of Kes 17 there are not signatures of carbon monoxide emissions above 3sigma, despite previously reported infrared observations have revealed shocked molecular gas at that location. This suggests the existence of a CO-dark interacting molecular gas, a phenomenon also recorded in other Galactic SNRs (e.g. CTB 37A and RX J1713.7-3946) brightening both in the infrared and gamma-ray domains. Additionally, by analysing ~14.5 yr of continuously collected data from the Large Area Telescope on board the satellite Fermi, we determined that the best-fit power-law photon index for the 0.3-300 GeV gamma-ray emission from the Kes 17 region is Gamma = 2.39 +/- 0.04 +0.063 -0.114 (+/-stat +/-syst) in agreement with prior studies. The energy flux turns out to be (2.98 +/- 0.14) x 10^-11 erg cm-2 s-1 implying a luminosity (2.22 +/- 0.45) x 10^35 erg s-1 at ~ 8 kpc. Finally, we successfully modelled the multiwavelength spectral energy distribution by incorporating the radio synchrotron spectrum and the new measurements of GeV gamma-rays. Our analysis indicates that the observed gamma-ray flux most likely originates from the interaction of Kes 17 with western "dark" CO zone with a proton density np ~400 cm-3.
Fil: Supán, Jorge Leonardo. Consejo Nacional de Investigaciones 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: Castelletti, Gabriela Marta. Consejo Nacional de Investigaciones 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: Lemiere, A.. Centre National de la Recherche Scientifique; Francia
description This paper presents a comprehensive analysis of the Galactic supernova remnant (SNR) Kes 17 (G304.6+0.1) with a focus on its radio synchrotron emission, environs, and the factors contributing to the observed gamma rays. The fitting to the firstly-obtained integrated radio continuum spectrum spanning from 88 to 8800 MHz yields an index alpha = -0.488 +/- 0.023 (S propto nu^alpha), indicative of a linear particle acceleration process at the shock front of the remnant. Accounting for the SNR radio shell size, the distribution of atomic hydrogen (nH ~ 10 cm-3), and assuming the SNR is in the Sedov-Taylor stage of its evolution, we estimate the remnant’s age to be roughly 8.5 kyr. This result falls at the lower end of the wide range (~2-64 kyr) derived from previous analyses of the diffuse X-ray emission interior to the remnant. Furthermore, we used 12CO and 13CO (J=1-0) emission-line data as a proxy for molecular hydrogen and provided the first evidence that the eastern shell of Kes 17 is engulfing a molecular enhancement in the surrounding gas, with an average mass 4.2 x 10^4 Msun and density n ~ 300 cm-3. Towards the western boundary of Kes 17 there are not signatures of carbon monoxide emissions above 3sigma, despite previously reported infrared observations have revealed shocked molecular gas at that location. This suggests the existence of a CO-dark interacting molecular gas, a phenomenon also recorded in other Galactic SNRs (e.g. CTB 37A and RX J1713.7-3946) brightening both in the infrared and gamma-ray domains. Additionally, by analysing ~14.5 yr of continuously collected data from the Large Area Telescope on board the satellite Fermi, we determined that the best-fit power-law photon index for the 0.3-300 GeV gamma-ray emission from the Kes 17 region is Gamma = 2.39 +/- 0.04 +0.063 -0.114 (+/-stat +/-syst) in agreement with prior studies. The energy flux turns out to be (2.98 +/- 0.14) x 10^-11 erg cm-2 s-1 implying a luminosity (2.22 +/- 0.45) x 10^35 erg s-1 at ~ 8 kpc. Finally, we successfully modelled the multiwavelength spectral energy distribution by incorporating the radio synchrotron spectrum and the new measurements of GeV gamma-rays. Our analysis indicates that the observed gamma-ray flux most likely originates from the interaction of Kes 17 with western "dark" CO zone with a proton density np ~400 cm-3.
publishDate 2023
dc.date.none.fl_str_mv 2023-07
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/11336/235586
Supán, Jorge Leonardo; Castelletti, Gabriela Marta; Lemiere, A.; The interaction of SNR Kes 17 with the interstellar medium: Fresh view from radio and γ-rays; EDP Sciences; Astronomy and Astrophysics; 679; 7-2023; 1-10
1432-0746
CONICET Digital
CONICET
url http://hdl.handle.net/11336/235586
identifier_str_mv Supán, Jorge Leonardo; Castelletti, Gabriela Marta; Lemiere, A.; The interaction of SNR Kes 17 with the interstellar medium: Fresh view from radio and γ-rays; EDP Sciences; Astronomy and Astrophysics; 679; 7-2023; 1-10
1432-0746
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/pdf/2023/11/aa47305-23.pdf
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202347305
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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