GS100-02-41: a new large H i shell in the outer part of the Galaxy

Autores
Suad, Laura Andrea; Cichowolski, Silvina; Arnal, Edmundo Marcelo; Testori, Juan Carlos
Año de publicación
2012
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. Massive stars have a profound effect on the surrounding interstellar medium. They ionize and heat the neutral gas, and with their strong winds they sweep up the gas, forming large H i shells. In this way, they generate a dense shell that provides the physical conditions for the formation of new stars. Aims: The aim of this study is to analyze the origin and evolution of the large H i shell GS 100-02-41 and its role in triggering star-forming processes. Methods: To characterize the shell and its environs, we carried out a multi-wavelength study. We analyzed the H i 21 cm line, the radio continuum, and infrared emission distributions. Results: The analysis of the H i data shows an expanding shell structure centered at (l,b) = (100°.6, -2°.04) in the velocity range from -29 to -51.7 km s-1. Taking into account noncircular motions, we infer for GS 100-02-41 a kinematical distance of 2.8 ± 0.6 kpc. Several massive stars belonging to Cep OB1 are located in projection within the large H i shell boundaries. The analysis of the radio continuum and infrared data reveals that there is no continuum counterpart of the H i shell. On the other hand, three slightly extended radio continuum sources are observed in projection onto the dense H i shell. From their flux density determinations we infer that they are thermal in nature. An analysis of the H i emission distribution in the environs of these sources shows a region of low emissivity for each of them, which correlates well morphologically with the ionized gas in a velocity range similar to the one where GS 100-02-41 is detected. Conclusions: Based on an energy analysis, we conclude that the origin of GS 100-02-41 could have been mainly caused by the action of the Cep OB1 massive stars located inside the H i shell. The obtained age difference between the H i shell and the H ii regions, together with their relative location, lead us to conclude that the ionizing stars could have been created as a consequence of the shell evolution.
Fil: Suad, Laura Andrea. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Cichowolski, Silvina. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Arnal, Edmundo Marcelo. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Testori, Juan Carlos. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Materia
ISM: structure
ISM: kinematics and dynamics
HII regions
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:11336/138531
Acceder
id CONICETDig_1f269484aac36747c6738c9624751677
oai_identifier_str oai:ri.conicet.gov.ar:11336/138531
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling GS100-02-41: a new large H i shell in the outer part of the GalaxySuad, Laura AndreaCichowolski, SilvinaArnal, Edmundo MarceloTestori, Juan CarlosISM: structureISM: kinematics and dynamicsHII regionsstars: formationhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. Massive stars have a profound effect on the surrounding interstellar medium. They ionize and heat the neutral gas, and with their strong winds they sweep up the gas, forming large H i shells. In this way, they generate a dense shell that provides the physical conditions for the formation of new stars. Aims: The aim of this study is to analyze the origin and evolution of the large H i shell GS 100-02-41 and its role in triggering star-forming processes. Methods: To characterize the shell and its environs, we carried out a multi-wavelength study. We analyzed the H i 21 cm line, the radio continuum, and infrared emission distributions. Results: The analysis of the H i data shows an expanding shell structure centered at (l,b) = (100°.6, -2°.04) in the velocity range from -29 to -51.7 km s-1. Taking into account noncircular motions, we infer for GS 100-02-41 a kinematical distance of 2.8 ± 0.6 kpc. Several massive stars belonging to Cep OB1 are located in projection within the large H i shell boundaries. The analysis of the radio continuum and infrared data reveals that there is no continuum counterpart of the H i shell. On the other hand, three slightly extended radio continuum sources are observed in projection onto the dense H i shell. From their flux density determinations we infer that they are thermal in nature. An analysis of the H i emission distribution in the environs of these sources shows a region of low emissivity for each of them, which correlates well morphologically with the ionized gas in a velocity range similar to the one where GS 100-02-41 is detected. Conclusions: Based on an energy analysis, we conclude that the origin of GS 100-02-41 could have been mainly caused by the action of the Cep OB1 massive stars located inside the H i shell. The obtained age difference between the H i shell and the H ii regions, together with their relative location, lead us to conclude that the ionizing stars could have been created as a consequence of the shell evolution.Fil: Suad, Laura Andrea. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaFil: Cichowolski, Silvina. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaFil: Arnal, Edmundo Marcelo. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaFil: Testori, Juan Carlos. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; ArgentinaEDP Sciences2012-02info: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/11336/138531Suad, Laura Andrea; Cichowolski, Silvina; Arnal, Edmundo Marcelo; Testori, Juan Carlos; GS100-02-41: a new large H i shell in the outer part of the Galaxy; EDP Sciences; Astronomy and Astrophysics; 538; A60; 2-2012; 60-690004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201118087info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2012/02/aa18087-11/aa18087-11.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 Técnicas2025-10-15T15:40:59Zoai:ri.conicet.gov.ar:11336/138531instacron: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:34982025-10-15 15:40:59.763CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv GS100-02-41: a new large H i shell in the outer part of the Galaxy
title GS100-02-41: a new large H i shell in the outer part of the Galaxy
spellingShingle GS100-02-41: a new large H i shell in the outer part of the Galaxy
Suad, Laura Andrea
ISM: structure
ISM: kinematics and dynamics
HII regions
stars: formation
title_short GS100-02-41: a new large H i shell in the outer part of the Galaxy
title_full GS100-02-41: a new large H i shell in the outer part of the Galaxy
title_fullStr GS100-02-41: a new large H i shell in the outer part of the Galaxy
title_full_unstemmed GS100-02-41: a new large H i shell in the outer part of the Galaxy
title_sort GS100-02-41: a new large H i shell in the outer part of the Galaxy
dc.creator.none.fl_str_mv Suad, Laura Andrea
Cichowolski, Silvina
Arnal, Edmundo Marcelo
Testori, Juan Carlos
author Suad, Laura Andrea
author_facet Suad, Laura Andrea
Cichowolski, Silvina
Arnal, Edmundo Marcelo
Testori, Juan Carlos
author_role author
author2 Cichowolski, Silvina
Arnal, Edmundo Marcelo
Testori, Juan Carlos
author2_role author
author
author
dc.subject.none.fl_str_mv ISM: structure
ISM: kinematics and dynamics
HII regions
stars: formation
topic ISM: structure
ISM: kinematics and dynamics
HII regions
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 Context. Massive stars have a profound effect on the surrounding interstellar medium. They ionize and heat the neutral gas, and with their strong winds they sweep up the gas, forming large H i shells. In this way, they generate a dense shell that provides the physical conditions for the formation of new stars. Aims: The aim of this study is to analyze the origin and evolution of the large H i shell GS 100-02-41 and its role in triggering star-forming processes. Methods: To characterize the shell and its environs, we carried out a multi-wavelength study. We analyzed the H i 21 cm line, the radio continuum, and infrared emission distributions. Results: The analysis of the H i data shows an expanding shell structure centered at (l,b) = (100°.6, -2°.04) in the velocity range from -29 to -51.7 km s-1. Taking into account noncircular motions, we infer for GS 100-02-41 a kinematical distance of 2.8 ± 0.6 kpc. Several massive stars belonging to Cep OB1 are located in projection within the large H i shell boundaries. The analysis of the radio continuum and infrared data reveals that there is no continuum counterpart of the H i shell. On the other hand, three slightly extended radio continuum sources are observed in projection onto the dense H i shell. From their flux density determinations we infer that they are thermal in nature. An analysis of the H i emission distribution in the environs of these sources shows a region of low emissivity for each of them, which correlates well morphologically with the ionized gas in a velocity range similar to the one where GS 100-02-41 is detected. Conclusions: Based on an energy analysis, we conclude that the origin of GS 100-02-41 could have been mainly caused by the action of the Cep OB1 massive stars located inside the H i shell. The obtained age difference between the H i shell and the H ii regions, together with their relative location, lead us to conclude that the ionizing stars could have been created as a consequence of the shell evolution.
Fil: Suad, Laura Andrea. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Cichowolski, Silvina. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Arnal, Edmundo Marcelo. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
Fil: Testori, Juan Carlos. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
description Context. Massive stars have a profound effect on the surrounding interstellar medium. They ionize and heat the neutral gas, and with their strong winds they sweep up the gas, forming large H i shells. In this way, they generate a dense shell that provides the physical conditions for the formation of new stars. Aims: The aim of this study is to analyze the origin and evolution of the large H i shell GS 100-02-41 and its role in triggering star-forming processes. Methods: To characterize the shell and its environs, we carried out a multi-wavelength study. We analyzed the H i 21 cm line, the radio continuum, and infrared emission distributions. Results: The analysis of the H i data shows an expanding shell structure centered at (l,b) = (100°.6, -2°.04) in the velocity range from -29 to -51.7 km s-1. Taking into account noncircular motions, we infer for GS 100-02-41 a kinematical distance of 2.8 ± 0.6 kpc. Several massive stars belonging to Cep OB1 are located in projection within the large H i shell boundaries. The analysis of the radio continuum and infrared data reveals that there is no continuum counterpart of the H i shell. On the other hand, three slightly extended radio continuum sources are observed in projection onto the dense H i shell. From their flux density determinations we infer that they are thermal in nature. An analysis of the H i emission distribution in the environs of these sources shows a region of low emissivity for each of them, which correlates well morphologically with the ionized gas in a velocity range similar to the one where GS 100-02-41 is detected. Conclusions: Based on an energy analysis, we conclude that the origin of GS 100-02-41 could have been mainly caused by the action of the Cep OB1 massive stars located inside the H i shell. The obtained age difference between the H i shell and the H ii regions, together with their relative location, lead us to conclude that the ionizing stars could have been created as a consequence of the shell evolution.
publishDate 2012
dc.date.none.fl_str_mv 2012-02
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/11336/138531
Suad, Laura Andrea; Cichowolski, Silvina; Arnal, Edmundo Marcelo; Testori, Juan Carlos; GS100-02-41: a new large H i shell in the outer part of the Galaxy; EDP Sciences; Astronomy and Astrophysics; 538; A60; 2-2012; 60-69
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/138531
identifier_str_mv Suad, Laura Andrea; Cichowolski, Silvina; Arnal, Edmundo Marcelo; Testori, Juan Carlos; GS100-02-41: a new large H i shell in the outer part of the Galaxy; EDP Sciences; Astronomy and Astrophysics; 538; A60; 2-2012; 60-69
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/10.1051/0004-6361/201118087
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2012/02/aa18087-11/aa18087-11.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 13.22299

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