Study of the molecular clump associated with the high-energy source HESS J1858+020

Autores
Paron, Sergio Ariel; Giacani, Elsa Beatriz; Rubio, M.; Dubner, Gloria Mabel
Año de publicación
2011
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Aims. HESS J1858+020 is a weak γ-ray source lying near the southern border of the SNR G35.6-0.4. A molecular cloud, composed of two clumps, shows signs of interaction with both the SNR and a nearby extended HII region. In particular, the southernmost clump coincides with the center of the H.E.S.S. source. We study this clump in detail to help us identify the nature of the very-high energy emission. Methods. We observed the aforementioned molecular clump using the Atacama Submillimeter Telescope Experiment (ASTE) in the 12CO J = 3−2, 13CO J = 3−2, HCO+J = 4−3, and CS J = 7−6 lines with an angular resolution of 22′′. To complement these observations, we analyzed IR and submillimeter continuum archival data. Results. From the 12CO and 13CO J = 3−2 lines and the 1.1 mm continuum emission, we derive a density of between 103 and 4 cm-3 for the clump. We discover a young stellar object (YSO), probably a high mass protostar, embedded in the molecular clump. However, we do not find any evidence of molecular outflows from this YSO that would represent a thermal jet capable of generating the observed γ-rays. We conclude that the most probable origin of the TeV γ-ray emission is a hadronic interaction between the molecular gas and the cosmic rays accelerated by the shock front of the SNR G35.6-0.4.
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
Fil: Rubio, M.. Universidad de Chile; Chile
Fil: Dubner, Gloria Mabel. 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: individual objects:HESS1858+020
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:11336/19902
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/19902
network_acronym_str CONICETDig
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network_name_str CONICET Digital (CONICET)
spelling Study of the molecular clump associated with the high-energy source HESS J1858+020Paron, Sergio ArielGiacani, Elsa BeatrizRubio, M.Dubner, Gloria MabelISM:cloudsISM:supernova remnants, gamma raysISM: individual objects:HESS1858+020https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Aims. HESS J1858+020 is a weak γ-ray source lying near the southern border of the SNR G35.6-0.4. A molecular cloud, composed of two clumps, shows signs of interaction with both the SNR and a nearby extended HII region. In particular, the southernmost clump coincides with the center of the H.E.S.S. source. We study this clump in detail to help us identify the nature of the very-high energy emission. Methods. We observed the aforementioned molecular clump using the Atacama Submillimeter Telescope Experiment (ASTE) in the 12CO J = 3−2, 13CO J = 3−2, HCO+J = 4−3, and CS J = 7−6 lines with an angular resolution of 22′′. To complement these observations, we analyzed IR and submillimeter continuum archival data. Results. From the 12CO and 13CO J = 3−2 lines and the 1.1 mm continuum emission, we derive a density of between 103 and 4 cm-3 for the clump. We discover a young stellar object (YSO), probably a high mass protostar, embedded in the molecular clump. However, we do not find any evidence of molecular outflows from this YSO that would represent a thermal jet capable of generating the observed γ-rays. We conclude that the most probable origin of the TeV γ-ray emission is a hadronic interaction between the molecular gas and the cosmic rays accelerated by the shock front of the SNR G35.6-0.4.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; ArgentinaFil: Rubio, M.. Universidad de Chile; ChileFil: Dubner, Gloria Mabel. 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 Sciences2011-06info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/19902Paron, Sergio Ariel; Giacani, Elsa Beatriz; Rubio, M.; Dubner, Gloria Mabel; Study of the molecular clump associated with the high-energy source HESS J1858+020; EDP Sciences; Astronomy and Astrophysics; 530; 6-2011; 1-6; A250004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201016390info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1103.5742info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2011/06/aa16390-10/aa16390-10.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 Técnicas2025-09-29T09:38:48Zoai:ri.conicet.gov.ar:11336/19902instacron: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 09:38:48.944CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Study of the molecular clump associated with the high-energy source HESS J1858+020
title Study of the molecular clump associated with the high-energy source HESS J1858+020
spellingShingle Study of the molecular clump associated with the high-energy source HESS J1858+020
Paron, Sergio Ariel
ISM:clouds
ISM:supernova remnants, gamma rays
ISM: individual objects:HESS1858+020
title_short Study of the molecular clump associated with the high-energy source HESS J1858+020
title_full Study of the molecular clump associated with the high-energy source HESS J1858+020
title_fullStr Study of the molecular clump associated with the high-energy source HESS J1858+020
title_full_unstemmed Study of the molecular clump associated with the high-energy source HESS J1858+020
title_sort Study of the molecular clump associated with the high-energy source HESS J1858+020
dc.creator.none.fl_str_mv Paron, Sergio Ariel
Giacani, Elsa Beatriz
Rubio, M.
Dubner, Gloria Mabel
author Paron, Sergio Ariel
author_facet Paron, Sergio Ariel
Giacani, Elsa Beatriz
Rubio, M.
Dubner, Gloria Mabel
author_role author
author2 Giacani, Elsa Beatriz
Rubio, M.
Dubner, Gloria Mabel
author2_role author
author
author
dc.subject.none.fl_str_mv ISM:clouds
ISM:supernova remnants, gamma rays
ISM: individual objects:HESS1858+020
topic ISM:clouds
ISM:supernova remnants, gamma rays
ISM: individual objects:HESS1858+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 lying near the southern border of the SNR G35.6-0.4. A molecular cloud, composed of two clumps, shows signs of interaction with both the SNR and a nearby extended HII region. In particular, the southernmost clump coincides with the center of the H.E.S.S. source. We study this clump in detail to help us identify the nature of the very-high energy emission. Methods. We observed the aforementioned molecular clump using the Atacama Submillimeter Telescope Experiment (ASTE) in the 12CO J = 3−2, 13CO J = 3−2, HCO+J = 4−3, and CS J = 7−6 lines with an angular resolution of 22′′. To complement these observations, we analyzed IR and submillimeter continuum archival data. Results. From the 12CO and 13CO J = 3−2 lines and the 1.1 mm continuum emission, we derive a density of between 103 and 4 cm-3 for the clump. We discover a young stellar object (YSO), probably a high mass protostar, embedded in the molecular clump. However, we do not find any evidence of molecular outflows from this YSO that would represent a thermal jet capable of generating the observed γ-rays. We conclude that the most probable origin of the TeV γ-ray emission is a hadronic interaction between the molecular gas and the cosmic rays accelerated by the shock front of the SNR G35.6-0.4.
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
Fil: Rubio, M.. Universidad de Chile; Chile
Fil: Dubner, Gloria Mabel. 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 lying near the southern border of the SNR G35.6-0.4. A molecular cloud, composed of two clumps, shows signs of interaction with both the SNR and a nearby extended HII region. In particular, the southernmost clump coincides with the center of the H.E.S.S. source. We study this clump in detail to help us identify the nature of the very-high energy emission. Methods. We observed the aforementioned molecular clump using the Atacama Submillimeter Telescope Experiment (ASTE) in the 12CO J = 3−2, 13CO J = 3−2, HCO+J = 4−3, and CS J = 7−6 lines with an angular resolution of 22′′. To complement these observations, we analyzed IR and submillimeter continuum archival data. Results. From the 12CO and 13CO J = 3−2 lines and the 1.1 mm continuum emission, we derive a density of between 103 and 4 cm-3 for the clump. We discover a young stellar object (YSO), probably a high mass protostar, embedded in the molecular clump. However, we do not find any evidence of molecular outflows from this YSO that would represent a thermal jet capable of generating the observed γ-rays. We conclude that the most probable origin of the TeV γ-ray emission is a hadronic interaction between the molecular gas and the cosmic rays accelerated by the shock front of the SNR G35.6-0.4.
publishDate 2011
dc.date.none.fl_str_mv 2011-06
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/11336/19902
Paron, Sergio Ariel; Giacani, Elsa Beatriz; Rubio, M.; Dubner, Gloria Mabel; Study of the molecular clump associated with the high-energy source HESS J1858+020; EDP Sciences; Astronomy and Astrophysics; 530; 6-2011; 1-6; A25
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/19902
identifier_str_mv Paron, Sergio Ariel; Giacani, Elsa Beatriz; Rubio, M.; Dubner, Gloria Mabel; Study of the molecular clump associated with the high-energy source HESS J1858+020; EDP Sciences; Astronomy and Astrophysics; 530; 6-2011; 1-6; A25
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/10.1051/0004-6361/201016390
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1103.5742
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2011/06/aa16390-10/aa16390-10.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
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 13.070432

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