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.
Facultad de Ciencias Astronómicas y Geofísicas - Materia
-
Ciencias Astronómicas
HII regions
ISM: kinematics and dynamics
ISM: structure
stars: formation - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/84123
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GS100-02-41: a new large H i shell in the outer part of the galaxySuad, Laura AndreaCichowolski, SilvinaArnal, Edmundo MarceloTestori, Juan CarlosCiencias AstronómicasHII regionsISM: kinematics and dynamicsISM: structurestars: formationContext. 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.Facultad de Ciencias Astronómicas y Geofísicas2012info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/84123enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201118087info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:16:05Zoai:sedici.unlp.edu.ar:10915/84123Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:05.506SEDICI (UNLP) - Universidad Nacional de La Platafalse |
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 Ciencias Astronómicas HII regions ISM: kinematics and dynamics ISM: structure 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 |
Ciencias Astronómicas HII regions ISM: kinematics and dynamics ISM: structure stars: formation |
topic |
Ciencias Astronómicas HII regions ISM: kinematics and dynamics ISM: structure stars: formation |
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. Facultad de Ciencias Astronómicas y Geofísicas |
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 |
dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion Articulo http://purl.org/coar/resource_type/c_6501 info:ar-repo/semantics/articulo |
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eng |
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http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) |
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