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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/17849
Ver los metadatos del registro completo
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oai:ri.conicet.gov.ar:11336/17849 |
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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 Técnicas2025-09-29T10:41:03Zoai: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:34982025-09-29 10:41:03.549CONICET 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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1844614440478048256 |
score |
13.070432 |