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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/20006
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oai:ri.conicet.gov.ar:11336/20006 |
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3498 |
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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 Técnicas2025-09-29T10:11:03Zoai: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:34982025-09-29 10:11:04.107CONICET 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 |
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reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) |
collection |
CONICET Digital (CONICET) |
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Consejo Nacional de Investigaciones Científicas y Técnicas |
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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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1844614005945008128 |
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13.070432 |