H II Region G46.5-0.2: The Interplay between Ionizing Radiation, Molecular Gas, and Star Formation

Autores
Paron, Sergio Ariel; Ortega, Martin Eduardo; Dubner, Gloria Mabel; Yuan, Jing-Hua; Petriella, Alberto; Giacani, Elsa Beatriz; Li, Jin Zeng; Wu, Yuefang; Liu, Hongli; Huang, Ya Fang; Zhang, Si-Ju
Año de publicación
2015
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
H ii regions are particularly interesting because they can generate dense layers of gas and dust, elongated columns or pillars of gas pointing toward the ionizing sources, and cometary globules of dense gas where triggered star formation can occur. Understanding the interplay between the ionizing radiation and the dense surrounding gas is very important to explain the origin of these peculiar structures, and hence to characterize triggered star formation. G46.5-0.2 (G46), a poorly studied galactic H ii region located at about 4 kpc, is an excellent target for performing this kind of study. Using public molecular data extracted from the Galactic Ring Survey (13CO J = 1?0) and from the James Clerk Maxwell Telescope data archive (12CO, 13CO, C18O J = 3?2, HCO+, and HCN J = 4?3), and infrared data from the GLIMPSE and MIPSGAL surveys, we perform a complete study of G46, its molecular environment, and the young stellar objects (YSOs) placed around it. We found that G46, probably excited by an O7V star, is located close to the edge of the GRSMC G046.34-00.21 molecular cloud. It presents a horse-shoe morphology opening in the direction of the cloud. We observed a filamentary structure in the molecular gas likely related to G46 and not considerable molecular emission toward its open border. We found that about 10‧ to the southwest of G46 there are some pillar-like features, shining at 8 μm and pointing toward the H ii region open border. We propose that the pillar-like features were carved and sculpted by the ionizing flux from G46. We found several YSOs likely embedded in the molecular cloud grouped in two main concentrations: one, closer to the G46 open border consisting of Class II type sources, and another mostly composed of Class I type YSOs located just ahead of the pillar-like features, strongly suggesting an age gradient in the YSO distribution.
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: Ortega, Martin Eduardo. 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: 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
Fil: Yuan, Jing-Hua. Chinese Academy of Sciences; China
Fil: Petriella, Alberto. 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: Li, Jin Zeng. Chinese Academy of Sciences; China
Fil: Wu, Yuefang. Peking University; China
Fil: Liu, Hongli. Chinese Academy of Sciences; China
Fil: Huang, Ya Fang. Chinese Academy of Sciences; China
Fil: Zhang, Si-Ju. Chinese Academy Of Sciences; República de China
Materia
Hii Regions
Ism: Clouds
Ism: Molecules
Stars: Formation
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:11336/17849
Acceder
id CONICETDig_40595a198721f41c1f9ffcbb1bbc63de
oai_identifier_str oai:ri.conicet.gov.ar:11336/17849
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling H II Region G46.5-0.2: The Interplay between Ionizing Radiation, Molecular Gas, and Star FormationParon, Sergio ArielOrtega, Martin EduardoDubner, Gloria MabelYuan, Jing-HuaPetriella, AlbertoGiacani, Elsa BeatrizLi, Jin ZengWu, YuefangLiu, HongliHuang, Ya FangZhang, Si-JuHii RegionsIsm: CloudsIsm: MoleculesStars: Formationhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1H ii regions are particularly interesting because they can generate dense layers of gas and dust, elongated columns or pillars of gas pointing toward the ionizing sources, and cometary globules of dense gas where triggered star formation can occur. Understanding the interplay between the ionizing radiation and the dense surrounding gas is very important to explain the origin of these peculiar structures, and hence to characterize triggered star formation. G46.5-0.2 (G46), a poorly studied galactic H ii region located at about 4 kpc, is an excellent target for performing this kind of study. Using public molecular data extracted from the Galactic Ring Survey (13CO J = 1?0) and from the James Clerk Maxwell Telescope data archive (12CO, 13CO, C18O J = 3?2, HCO+, and HCN J = 4?3), and infrared data from the GLIMPSE and MIPSGAL surveys, we perform a complete study of G46, its molecular environment, and the young stellar objects (YSOs) placed around it. We found that G46, probably excited by an O7V star, is located close to the edge of the GRSMC G046.34-00.21 molecular cloud. It presents a horse-shoe morphology opening in the direction of the cloud. We observed a filamentary structure in the molecular gas likely related to G46 and not considerable molecular emission toward its open border. We found that about 10‧ to the southwest of G46 there are some pillar-like features, shining at 8 μm and pointing toward the H ii region open border. We propose that the pillar-like features were carved and sculpted by the ionizing flux from G46. We found several YSOs likely embedded in the molecular cloud grouped in two main concentrations: one, closer to the G46 open border consisting of Class II type sources, and another mostly composed of Class I type YSOs located just ahead of the pillar-like features, strongly suggesting an age gradient in the YSO distribution.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: Ortega, Martin Eduardo. 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: 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; ArgentinaFil: Yuan, Jing-Hua. Chinese Academy of Sciences; ChinaFil: Petriella, Alberto. 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: Li, Jin Zeng. Chinese Academy of Sciences; ChinaFil: Wu, Yuefang. Peking University; ChinaFil: Liu, Hongli. Chinese Academy of Sciences; ChinaFil: Huang, Ya Fang. Chinese Academy of Sciences; ChinaFil: Zhang, Si-Ju. Chinese Academy Of Sciences; República de ChinaIop Publishing2015-06info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/17849Paron, Sergio Ariel; Ortega, Martin Eduardo; Dubner, Gloria Mabel; Yuan, Jing-Hua; Petriella, Alberto; et al.; H II Region G46.5-0.2: The Interplay between Ionizing Radiation, Molecular Gas, and Star Formation; Iop Publishing; Astronomical Journal; 149; 6-2015; 193,1-110004-6256enginfo:eu-repo/semantics/altIdentifier/doi/10.1088/0004-6256/149/6/193info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1504.03935info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0004-6256/149/6/193/metainfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T12:13:34Zoai:ri.conicet.gov.ar:11336/17849instacron: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 12:13:34.635CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv H II Region G46.5-0.2: The Interplay between Ionizing Radiation, Molecular Gas, and Star Formation
title H II Region G46.5-0.2: The Interplay between Ionizing Radiation, Molecular Gas, and Star Formation
spellingShingle H II Region G46.5-0.2: The Interplay between Ionizing Radiation, Molecular Gas, and Star Formation
Paron, Sergio Ariel
Hii Regions
Ism: Clouds
Ism: Molecules
Stars: Formation
title_short H II Region G46.5-0.2: The Interplay between Ionizing Radiation, Molecular Gas, and Star Formation
title_full H II Region G46.5-0.2: The Interplay between Ionizing Radiation, Molecular Gas, and Star Formation
title_fullStr H II Region G46.5-0.2: The Interplay between Ionizing Radiation, Molecular Gas, and Star Formation
title_full_unstemmed H II Region G46.5-0.2: The Interplay between Ionizing Radiation, Molecular Gas, and Star Formation
title_sort H II Region G46.5-0.2: The Interplay between Ionizing Radiation, Molecular Gas, and Star Formation
dc.creator.none.fl_str_mv Paron, Sergio Ariel
Ortega, Martin Eduardo
Dubner, Gloria Mabel
Yuan, Jing-Hua
Petriella, Alberto
Giacani, Elsa Beatriz
Li, Jin Zeng
Wu, Yuefang
Liu, Hongli
Huang, Ya Fang
Zhang, Si-Ju
author Paron, Sergio Ariel
author_facet Paron, Sergio Ariel
Ortega, Martin Eduardo
Dubner, Gloria Mabel
Yuan, Jing-Hua
Petriella, Alberto
Giacani, Elsa Beatriz
Li, Jin Zeng
Wu, Yuefang
Liu, Hongli
Huang, Ya Fang
Zhang, Si-Ju
author_role author
author2 Ortega, Martin Eduardo
Dubner, Gloria Mabel
Yuan, Jing-Hua
Petriella, Alberto
Giacani, Elsa Beatriz
Li, Jin Zeng
Wu, Yuefang
Liu, Hongli
Huang, Ya Fang
Zhang, Si-Ju
author2_role author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv Hii Regions
Ism: Clouds
Ism: Molecules
Stars: Formation
topic Hii Regions
Ism: Clouds
Ism: Molecules
Stars: Formation
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv H ii regions are particularly interesting because they can generate dense layers of gas and dust, elongated columns or pillars of gas pointing toward the ionizing sources, and cometary globules of dense gas where triggered star formation can occur. Understanding the interplay between the ionizing radiation and the dense surrounding gas is very important to explain the origin of these peculiar structures, and hence to characterize triggered star formation. G46.5-0.2 (G46), a poorly studied galactic H ii region located at about 4 kpc, is an excellent target for performing this kind of study. Using public molecular data extracted from the Galactic Ring Survey (13CO J = 1?0) and from the James Clerk Maxwell Telescope data archive (12CO, 13CO, C18O J = 3?2, HCO+, and HCN J = 4?3), and infrared data from the GLIMPSE and MIPSGAL surveys, we perform a complete study of G46, its molecular environment, and the young stellar objects (YSOs) placed around it. We found that G46, probably excited by an O7V star, is located close to the edge of the GRSMC G046.34-00.21 molecular cloud. It presents a horse-shoe morphology opening in the direction of the cloud. We observed a filamentary structure in the molecular gas likely related to G46 and not considerable molecular emission toward its open border. We found that about 10‧ to the southwest of G46 there are some pillar-like features, shining at 8 μm and pointing toward the H ii region open border. We propose that the pillar-like features were carved and sculpted by the ionizing flux from G46. We found several YSOs likely embedded in the molecular cloud grouped in two main concentrations: one, closer to the G46 open border consisting of Class II type sources, and another mostly composed of Class I type YSOs located just ahead of the pillar-like features, strongly suggesting an age gradient in the YSO distribution.
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: Ortega, Martin Eduardo. 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: 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
Fil: Yuan, Jing-Hua. Chinese Academy of Sciences; China
Fil: Petriella, Alberto. 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: Li, Jin Zeng. Chinese Academy of Sciences; China
Fil: Wu, Yuefang. Peking University; China
Fil: Liu, Hongli. Chinese Academy of Sciences; China
Fil: Huang, Ya Fang. Chinese Academy of Sciences; China
Fil: Zhang, Si-Ju. Chinese Academy Of Sciences; República de China
description H ii regions are particularly interesting because they can generate dense layers of gas and dust, elongated columns or pillars of gas pointing toward the ionizing sources, and cometary globules of dense gas where triggered star formation can occur. Understanding the interplay between the ionizing radiation and the dense surrounding gas is very important to explain the origin of these peculiar structures, and hence to characterize triggered star formation. G46.5-0.2 (G46), a poorly studied galactic H ii region located at about 4 kpc, is an excellent target for performing this kind of study. Using public molecular data extracted from the Galactic Ring Survey (13CO J = 1?0) and from the James Clerk Maxwell Telescope data archive (12CO, 13CO, C18O J = 3?2, HCO+, and HCN J = 4?3), and infrared data from the GLIMPSE and MIPSGAL surveys, we perform a complete study of G46, its molecular environment, and the young stellar objects (YSOs) placed around it. We found that G46, probably excited by an O7V star, is located close to the edge of the GRSMC G046.34-00.21 molecular cloud. It presents a horse-shoe morphology opening in the direction of the cloud. We observed a filamentary structure in the molecular gas likely related to G46 and not considerable molecular emission toward its open border. We found that about 10‧ to the southwest of G46 there are some pillar-like features, shining at 8 μm and pointing toward the H ii region open border. We propose that the pillar-like features were carved and sculpted by the ionizing flux from G46. We found several YSOs likely embedded in the molecular cloud grouped in two main concentrations: one, closer to the G46 open border consisting of Class II type sources, and another mostly composed of Class I type YSOs located just ahead of the pillar-like features, strongly suggesting an age gradient in the YSO distribution.
publishDate 2015
dc.date.none.fl_str_mv 2015-06
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/11336/17849
Paron, Sergio Ariel; Ortega, Martin Eduardo; Dubner, Gloria Mabel; Yuan, Jing-Hua; Petriella, Alberto; et al.; H II Region G46.5-0.2: The Interplay between Ionizing Radiation, Molecular Gas, and Star Formation; Iop Publishing; Astronomical Journal; 149; 6-2015; 193,1-11
0004-6256
url http://hdl.handle.net/11336/17849
identifier_str_mv Paron, Sergio Ariel; Ortega, Martin Eduardo; Dubner, Gloria Mabel; Yuan, Jing-Hua; Petriella, Alberto; et al.; H II Region G46.5-0.2: The Interplay between Ionizing Radiation, Molecular Gas, and Star Formation; Iop Publishing; Astronomical Journal; 149; 6-2015; 193,1-11
0004-6256
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1088/0004-6256/149/6/193
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1504.03935
info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0004-6256/149/6/193/meta
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
application/pdf
dc.publisher.none.fl_str_mv Iop Publishing
publisher.none.fl_str_mv Iop Publishing
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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