Cosmic rays in the surroundings of SNR G35.6-0.4

Autores
Torres, Diego F.; Li, Hui; Chen, Yang; Cillis, Analia Nilda; Caliandro, Andrea G.; Rodríguez Marrero, Ana Y.
Año de publicación
2011
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
HESS J1858+020 is a TeV gamma-ray source that was reported not to have any clear cataloged counterpart at any wavelength. However, it has been recently proposed that this source is indirectly associated with the radio source, re-identified as a supernova remnant (SNR), G35.6-0.4. The latter is found to be middle-aged ($sim 30$ kyr) and to have nearby molecular clouds (MCs). HESS J1858+020 was proposed to be the result of the interaction of protons accelerated in the SNR shell with target ions residing in the clouds. The Fermi Large Area Telescope (LAT) First Source Catalog does not list any source coincident with the position of HESS J1858+020, but some lie close. Here, we analyse more than 2 years of data obtained with the Fermi-LAT for the region of interest, and consider whether it is indeed possible that the closest LAT source, 1FGL J1857.1+0212c, is related to HESS J1858+020. We conclude it is not, and we impose upper limits on the GeV emission originating from HESS J1858+020. Using a simplified 3D model for the cosmic-ray propagation out from the shell of the SNR, we consider whether the interaction between SNR G35.6-0.4 and the MCs nearby could give rise to the TeV emission of HESS J1858+020 without producing a GeV counterpart. If so, the pair of SNR/TeV source with no GeV detection would be reminiscent of other similarly-aged SNRs, such as some of the TeV hotspots near W28, for which cosmic-ray diffusion may be used to explain their multi-frequency phenomenology. However, for HESS J1858+020, we found that although the phase space in principle allows for such GeV--TeV non-correlation to appear, usual and/or observationally constrained values of the parameters (e.g., diffusion coefficients and cloud-SNR likely distances) would disfavor it.
Fil: Torres, Diego F.. Institució Catalana de Recerca I Estudis Avançats; España
Fil: Li, Hui. Nanjing University; China
Fil: Chen, Yang. Key Laboratory Of Modern Astronomy And Astrophysics; China. Nanjing University; China
Fil: Cillis, Analia Nilda. 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: Caliandro, Andrea G.. Institució Catalana de Recerca i Estudis Avancats; España
Fil: Rodríguez Marrero, Ana Y.. Instituto de Física de Cantabria; España
Materia
supernova remnants
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:11336/20006
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/20006
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Cosmic rays in the surroundings of SNR G35.6-0.4Torres, Diego F.Li, HuiChen, YangCillis, Analia NildaCaliandro, Andrea G.Rodríguez Marrero, Ana Y.supernova remnantshttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1HESS J1858+020 is a TeV gamma-ray source that was reported not to have any clear cataloged counterpart at any wavelength. However, it has been recently proposed that this source is indirectly associated with the radio source, re-identified as a supernova remnant (SNR), G35.6-0.4. The latter is found to be middle-aged ($sim 30$ kyr) and to have nearby molecular clouds (MCs). HESS J1858+020 was proposed to be the result of the interaction of protons accelerated in the SNR shell with target ions residing in the clouds. The Fermi Large Area Telescope (LAT) First Source Catalog does not list any source coincident with the position of HESS J1858+020, but some lie close. Here, we analyse more than 2 years of data obtained with the Fermi-LAT for the region of interest, and consider whether it is indeed possible that the closest LAT source, 1FGL J1857.1+0212c, is related to HESS J1858+020. We conclude it is not, and we impose upper limits on the GeV emission originating from HESS J1858+020. Using a simplified 3D model for the cosmic-ray propagation out from the shell of the SNR, we consider whether the interaction between SNR G35.6-0.4 and the MCs nearby could give rise to the TeV emission of HESS J1858+020 without producing a GeV counterpart. If so, the pair of SNR/TeV source with no GeV detection would be reminiscent of other similarly-aged SNRs, such as some of the TeV hotspots near W28, for which cosmic-ray diffusion may be used to explain their multi-frequency phenomenology. However, for HESS J1858+020, we found that although the phase space in principle allows for such GeV--TeV non-correlation to appear, usual and/or observationally constrained values of the parameters (e.g., diffusion coefficients and cloud-SNR likely distances) would disfavor it.Fil: Torres, Diego F.. Institució Catalana de Recerca I Estudis Avançats; EspañaFil: Li, Hui. Nanjing University; ChinaFil: Chen, Yang. Key Laboratory Of Modern Astronomy And Astrophysics; China. Nanjing University; ChinaFil: Cillis, Analia Nilda. 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: Caliandro, Andrea G.. Institució Catalana de Recerca i Estudis Avancats; EspañaFil: Rodríguez Marrero, Ana Y.. Instituto de Física de Cantabria; EspañaOxford University Press2011-11-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/20006Torres, Diego F.; Li, Hui; Chen, Yang; Cillis, Analia Nilda; Caliandro, Andrea G.; et al.; Cosmic rays in the surroundings of SNR G35.6-0.4; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 417; 4; 2-11-2011; 3072-30790035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/417/4/3072/1101823/Cosmic-rays-in-the-surroundings-of-SNR-G35-6-0-4info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2011.19465.xinfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1107.3470info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:41:01Zoai:ri.conicet.gov.ar:11336/20006instacron: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:34982025-10-22 11:41:01.453CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Cosmic rays in the surroundings of SNR G35.6-0.4
title Cosmic rays in the surroundings of SNR G35.6-0.4
spellingShingle Cosmic rays in the surroundings of SNR G35.6-0.4
Torres, Diego F.
supernova remnants
title_short Cosmic rays in the surroundings of SNR G35.6-0.4
title_full Cosmic rays in the surroundings of SNR G35.6-0.4
title_fullStr Cosmic rays in the surroundings of SNR G35.6-0.4
title_full_unstemmed Cosmic rays in the surroundings of SNR G35.6-0.4
title_sort Cosmic rays in the surroundings of SNR G35.6-0.4
dc.creator.none.fl_str_mv Torres, Diego F.
Li, Hui
Chen, Yang
Cillis, Analia Nilda
Caliandro, Andrea G.
Rodríguez Marrero, Ana Y.
author Torres, Diego F.
author_facet Torres, Diego F.
Li, Hui
Chen, Yang
Cillis, Analia Nilda
Caliandro, Andrea G.
Rodríguez Marrero, Ana Y.
author_role author
author2 Li, Hui
Chen, Yang
Cillis, Analia Nilda
Caliandro, Andrea G.
Rodríguez Marrero, Ana Y.
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv supernova remnants
topic supernova remnants
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv HESS J1858+020 is a TeV gamma-ray source that was reported not to have any clear cataloged counterpart at any wavelength. However, it has been recently proposed that this source is indirectly associated with the radio source, re-identified as a supernova remnant (SNR), G35.6-0.4. The latter is found to be middle-aged ($sim 30$ kyr) and to have nearby molecular clouds (MCs). HESS J1858+020 was proposed to be the result of the interaction of protons accelerated in the SNR shell with target ions residing in the clouds. The Fermi Large Area Telescope (LAT) First Source Catalog does not list any source coincident with the position of HESS J1858+020, but some lie close. Here, we analyse more than 2 years of data obtained with the Fermi-LAT for the region of interest, and consider whether it is indeed possible that the closest LAT source, 1FGL J1857.1+0212c, is related to HESS J1858+020. We conclude it is not, and we impose upper limits on the GeV emission originating from HESS J1858+020. Using a simplified 3D model for the cosmic-ray propagation out from the shell of the SNR, we consider whether the interaction between SNR G35.6-0.4 and the MCs nearby could give rise to the TeV emission of HESS J1858+020 without producing a GeV counterpart. If so, the pair of SNR/TeV source with no GeV detection would be reminiscent of other similarly-aged SNRs, such as some of the TeV hotspots near W28, for which cosmic-ray diffusion may be used to explain their multi-frequency phenomenology. However, for HESS J1858+020, we found that although the phase space in principle allows for such GeV--TeV non-correlation to appear, usual and/or observationally constrained values of the parameters (e.g., diffusion coefficients and cloud-SNR likely distances) would disfavor it.
Fil: Torres, Diego F.. Institució Catalana de Recerca I Estudis Avançats; España
Fil: Li, Hui. Nanjing University; China
Fil: Chen, Yang. Key Laboratory Of Modern Astronomy And Astrophysics; China. Nanjing University; China
Fil: Cillis, Analia Nilda. 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: Caliandro, Andrea G.. Institució Catalana de Recerca i Estudis Avancats; España
Fil: Rodríguez Marrero, Ana Y.. Instituto de Física de Cantabria; España
description HESS J1858+020 is a TeV gamma-ray source that was reported not to have any clear cataloged counterpart at any wavelength. However, it has been recently proposed that this source is indirectly associated with the radio source, re-identified as a supernova remnant (SNR), G35.6-0.4. The latter is found to be middle-aged ($sim 30$ kyr) and to have nearby molecular clouds (MCs). HESS J1858+020 was proposed to be the result of the interaction of protons accelerated in the SNR shell with target ions residing in the clouds. The Fermi Large Area Telescope (LAT) First Source Catalog does not list any source coincident with the position of HESS J1858+020, but some lie close. Here, we analyse more than 2 years of data obtained with the Fermi-LAT for the region of interest, and consider whether it is indeed possible that the closest LAT source, 1FGL J1857.1+0212c, is related to HESS J1858+020. We conclude it is not, and we impose upper limits on the GeV emission originating from HESS J1858+020. Using a simplified 3D model for the cosmic-ray propagation out from the shell of the SNR, we consider whether the interaction between SNR G35.6-0.4 and the MCs nearby could give rise to the TeV emission of HESS J1858+020 without producing a GeV counterpart. If so, the pair of SNR/TeV source with no GeV detection would be reminiscent of other similarly-aged SNRs, such as some of the TeV hotspots near W28, for which cosmic-ray diffusion may be used to explain their multi-frequency phenomenology. However, for HESS J1858+020, we found that although the phase space in principle allows for such GeV--TeV non-correlation to appear, usual and/or observationally constrained values of the parameters (e.g., diffusion coefficients and cloud-SNR likely distances) would disfavor it.
publishDate 2011
dc.date.none.fl_str_mv 2011-11-02
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/11336/20006
Torres, Diego F.; Li, Hui; Chen, Yang; Cillis, Analia Nilda; Caliandro, Andrea G.; et al.; Cosmic rays in the surroundings of SNR G35.6-0.4; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 417; 4; 2-11-2011; 3072-3079
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/20006
identifier_str_mv Torres, Diego F.; Li, Hui; Chen, Yang; Cillis, Analia Nilda; Caliandro, Andrea G.; et al.; Cosmic rays in the surroundings of SNR G35.6-0.4; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 417; 4; 2-11-2011; 3072-3079
0035-8711
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://academic.oup.com/mnras/article/417/4/3072/1101823/Cosmic-rays-in-the-surroundings-of-SNR-G35-6-0-4
info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2011.19465.x
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1107.3470
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 Oxford University Press
publisher.none.fl_str_mv Oxford University Press
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 12.982451

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