Identifying the counterpart of HESS J1858+020
- Autores
- Paron, Sergio Ariel; Giacani, Elsa Beatriz
- Año de publicación
- 2010
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Aims: HESS J1858+020 is a weak γ-ray source that does not have any clear cataloged counterpart at any wavelengths. Recently, the source G35.6-0.4 was re-identified as a SNR. The HESS source lies towards the southern border of this remnant. The purpose of this work is to investigate the interstellar medium around the mentioned sources to look for possible counterparts of the very high energy emission.
Methods: Using the 13CO J=1-0 line from the Galactic Ring Survey and mid-IR data from GLIMPSE we analyze the environs of HESS J1858+020 and SNR G35.6-0.4.
Results: The 13CO data show the presence of a molecular cloud towards the southern border of SNR G35.6-0.4 and at the same distance as the remnant. This cloud is composed of two molecular clumps, one over the SNR shell and the other located at the center of HESS J1858+020. We estimate a molecular mass and a density of ˜ 5 × 103 M_ȯ and ~500 cm-3 respectively for each clump. Considering the gamma-ray flux observed towards HESS J1858+020, we estimate that a molecular cloud with a density of at least 150 cm-3 could explain the very high energy emission hadronically. Thus, we suggest that the γ-ray emission detected in HESS J1858+020 is due to hadronic mechanism. Additionally, analyzing mid-IR emission, we find that the region is active in star formation, which could be considered as an alternative or complementary possibility to explain the very high energy emission.
Fil: Paron, Sergio Ariel. 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 - Materia
-
ISM:CLOUDS
ISM:SUPERNOVA REMNANTS
GAMMA RAYS: ISM
ISM:INDIVIDUAL OBJECTS:HESS J1858+020 - 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:11336/19026
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oai:ri.conicet.gov.ar:11336/19026 |
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CONICETDig |
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3498 |
network_name_str |
CONICET Digital (CONICET) |
spelling |
Identifying the counterpart of HESS J1858+020Paron, Sergio ArielGiacani, Elsa BeatrizISM:CLOUDSISM:SUPERNOVA REMNANTSGAMMA RAYS: ISMISM:INDIVIDUAL OBJECTS:HESS J1858+020https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Aims: HESS J1858+020 is a weak γ-ray source that does not have any clear cataloged counterpart at any wavelengths. Recently, the source G35.6-0.4 was re-identified as a SNR. The HESS source lies towards the southern border of this remnant. The purpose of this work is to investigate the interstellar medium around the mentioned sources to look for possible counterparts of the very high energy emission. <br /> Methods: Using the <sup>13</sup>CO J=1-0 line from the Galactic Ring Survey and mid-IR data from GLIMPSE we analyze the environs of HESS J1858+020 and SNR G35.6-0.4. <br /> Results: The <sup>13</sup>CO data show the presence of a molecular cloud towards the southern border of SNR G35.6-0.4 and at the same distance as the remnant. This cloud is composed of two molecular clumps, one over the SNR shell and the other located at the center of HESS J1858+020. We estimate a molecular mass and a density of ˜ 5 × 10<sup>3</sup> M_ȯ and ~500 cm<sup>-3</sup> respectively for each clump. Considering the gamma-ray flux observed towards HESS J1858+020, we estimate that a molecular cloud with a density of at least 150 cm<sup>-3</sup> could explain the very high energy emission hadronically. Thus, we suggest that the γ-ray emission detected in HESS J1858+020 is due to hadronic mechanism. Additionally, analyzing mid-IR emission, we find that the region is active in star formation, which could be considered as an alternative or complementary possibility to explain the very high energy emission.Fil: Paron, Sergio Ariel. 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; ArgentinaEDP Sciences2010-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/19026Paron, Sergio Ariel; Giacani, Elsa Beatriz; Identifying the counterpart of HESS J1858+020; EDP Sciences; Astronomy and Astrophysics; 509; L4; 1-2010; 1-30004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/200913694info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/0912.2669info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2010/01/aa13694-09/aa13694-09.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 Técnicas2025-09-29T09:47:16Zoai:ri.conicet.gov.ar:11336/19026instacron: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 09:47:17.105CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Identifying the counterpart of HESS J1858+020 |
title |
Identifying the counterpart of HESS J1858+020 |
spellingShingle |
Identifying the counterpart of HESS J1858+020 Paron, Sergio Ariel ISM:CLOUDS ISM:SUPERNOVA REMNANTS GAMMA RAYS: ISM ISM:INDIVIDUAL OBJECTS:HESS J1858+020 |
title_short |
Identifying the counterpart of HESS J1858+020 |
title_full |
Identifying the counterpart of HESS J1858+020 |
title_fullStr |
Identifying the counterpart of HESS J1858+020 |
title_full_unstemmed |
Identifying the counterpart of HESS J1858+020 |
title_sort |
Identifying the counterpart of HESS J1858+020 |
dc.creator.none.fl_str_mv |
Paron, Sergio Ariel Giacani, Elsa Beatriz |
author |
Paron, Sergio Ariel |
author_facet |
Paron, Sergio Ariel Giacani, Elsa Beatriz |
author_role |
author |
author2 |
Giacani, Elsa Beatriz |
author2_role |
author |
dc.subject.none.fl_str_mv |
ISM:CLOUDS ISM:SUPERNOVA REMNANTS GAMMA RAYS: ISM ISM:INDIVIDUAL OBJECTS:HESS J1858+020 |
topic |
ISM:CLOUDS ISM:SUPERNOVA REMNANTS GAMMA RAYS: ISM ISM:INDIVIDUAL OBJECTS:HESS J1858+020 |
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: HESS J1858+020 is a weak γ-ray source that does not have any clear cataloged counterpart at any wavelengths. Recently, the source G35.6-0.4 was re-identified as a SNR. The HESS source lies towards the southern border of this remnant. The purpose of this work is to investigate the interstellar medium around the mentioned sources to look for possible counterparts of the very high energy emission. <br /> Methods: Using the <sup>13</sup>CO J=1-0 line from the Galactic Ring Survey and mid-IR data from GLIMPSE we analyze the environs of HESS J1858+020 and SNR G35.6-0.4. <br /> Results: The <sup>13</sup>CO data show the presence of a molecular cloud towards the southern border of SNR G35.6-0.4 and at the same distance as the remnant. This cloud is composed of two molecular clumps, one over the SNR shell and the other located at the center of HESS J1858+020. We estimate a molecular mass and a density of ˜ 5 × 10<sup>3</sup> M_ȯ and ~500 cm<sup>-3</sup> respectively for each clump. Considering the gamma-ray flux observed towards HESS J1858+020, we estimate that a molecular cloud with a density of at least 150 cm<sup>-3</sup> could explain the very high energy emission hadronically. Thus, we suggest that the γ-ray emission detected in HESS J1858+020 is due to hadronic mechanism. Additionally, analyzing mid-IR emission, we find that the region is active in star formation, which could be considered as an alternative or complementary possibility to explain the very high energy emission. Fil: Paron, Sergio Ariel. 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 |
description |
Aims: HESS J1858+020 is a weak γ-ray source that does not have any clear cataloged counterpart at any wavelengths. Recently, the source G35.6-0.4 was re-identified as a SNR. The HESS source lies towards the southern border of this remnant. The purpose of this work is to investigate the interstellar medium around the mentioned sources to look for possible counterparts of the very high energy emission. <br /> Methods: Using the <sup>13</sup>CO J=1-0 line from the Galactic Ring Survey and mid-IR data from GLIMPSE we analyze the environs of HESS J1858+020 and SNR G35.6-0.4. <br /> Results: The <sup>13</sup>CO data show the presence of a molecular cloud towards the southern border of SNR G35.6-0.4 and at the same distance as the remnant. This cloud is composed of two molecular clumps, one over the SNR shell and the other located at the center of HESS J1858+020. We estimate a molecular mass and a density of ˜ 5 × 10<sup>3</sup> M_ȯ and ~500 cm<sup>-3</sup> respectively for each clump. Considering the gamma-ray flux observed towards HESS J1858+020, we estimate that a molecular cloud with a density of at least 150 cm<sup>-3</sup> could explain the very high energy emission hadronically. Thus, we suggest that the γ-ray emission detected in HESS J1858+020 is due to hadronic mechanism. Additionally, analyzing mid-IR emission, we find that the region is active in star formation, which could be considered as an alternative or complementary possibility to explain the very high energy emission. |
publishDate |
2010 |
dc.date.none.fl_str_mv |
2010-01 |
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/11336/19026 Paron, Sergio Ariel; Giacani, Elsa Beatriz; Identifying the counterpart of HESS J1858+020; EDP Sciences; Astronomy and Astrophysics; 509; L4; 1-2010; 1-3 0004-6361 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/19026 |
identifier_str_mv |
Paron, Sergio Ariel; Giacani, Elsa Beatriz; Identifying the counterpart of HESS J1858+020; EDP Sciences; Astronomy and Astrophysics; 509; L4; 1-2010; 1-3 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/doi/10.1051/0004-6361/200913694 info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/0912.2669 info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2010/01/aa13694-09/aa13694-09.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 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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1844613473631207424 |
score |
13.070432 |