Sh2-205 - I: the surrounding interstellar medium
- Autores
- Romero, Gisela Andrea; Cappa, Cristina Elisabet
- Año de publicación
- 2008
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We investigate the distribution of the interstellar matter in the environs of the H II region Sh2-205, based on neutral hydrogen 21-cm-line data and radio continuum images at 408 and 1420 MHz obtained from the CGPS, 12CO (J=1 →0) observations, high-resolution IRAS data (HIRES), and MSX data. Sh2-205 can be separated into three distinct optical structures: SH 149.25-0.0, SH 148.83-0.67, and LBN 148.11-0.45. The three regions are detected at both 408 and 1420 MHz. The derived spectral indices show the thermal nature of SH 148.83-0.67 and LBN 148.11-0.45. LBN 148.11-0.45 is a classical H II region surrounded by an H i shell. The associated neutral atomic and ionized masses are 65 M⊙ and 70 M⊙, respectively. Dust and molecular gas (∼6 × 104 M⊙) related to this ionized region have been found. In particular, a photodissociation region is detected at the interface between the ionized and molecular regions. If the proposed exciting star HD 24094 were an O8-O9 type star, as suggested by its near-infrared colours, its UV photon flux would be strong enough to explain the ionization of the nebula. The optical, radio continuum, and 21-cm-line data allow us to conclude that SH 148.83-0.67 is an interstellar bubble powered by the energetic action of HD 24431. The associated neutral atomic and ionized masses are 180 M⊙ and 300 M⊙, respectively. The emission of SH 149.25-0.0 is too faint to derive the dust and gas parameters. An H I shell centred at (l, b) = (149°0', -1°30') was also identified. It correlates morphologically with the molecular gas emission. The neutral atomic and molecular masses of the shell are 1600 M⊙ and 2.6 × 104 M⊙, respectively. The open cluster NGC 1444 is probably responsible for shaping this H I structure.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto Argentino de Radioastronomía - Materia
-
Ciencias Astronómicas
ISM: bubbles - ISM: structure
Stars: individual: ALS 7793
Stars: individual: HD 24094
Stars: individual: HD 24431 - 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:10915/84774
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Sh2-205 - I: the surrounding interstellar mediumRomero, Gisela AndreaCappa, Cristina ElisabetCiencias AstronómicasISM: bubbles - ISM: structureStars: individual: ALS 7793Stars: individual: HD 24094Stars: individual: HD 24431We investigate the distribution of the interstellar matter in the environs of the H II region Sh2-205, based on neutral hydrogen 21-cm-line data and radio continuum images at 408 and 1420 MHz obtained from the CGPS, 12CO (J=1 →0) observations, high-resolution IRAS data (HIRES), and MSX data. Sh2-205 can be separated into three distinct optical structures: SH 149.25-0.0, SH 148.83-0.67, and LBN 148.11-0.45. The three regions are detected at both 408 and 1420 MHz. The derived spectral indices show the thermal nature of SH 148.83-0.67 and LBN 148.11-0.45. LBN 148.11-0.45 is a classical H II region surrounded by an H i shell. The associated neutral atomic and ionized masses are 65 M⊙ and 70 M⊙, respectively. Dust and molecular gas (∼6 × 104 M⊙) related to this ionized region have been found. In particular, a photodissociation region is detected at the interface between the ionized and molecular regions. If the proposed exciting star HD 24094 were an O8-O9 type star, as suggested by its near-infrared colours, its UV photon flux would be strong enough to explain the ionization of the nebula. The optical, radio continuum, and 21-cm-line data allow us to conclude that SH 148.83-0.67 is an interstellar bubble powered by the energetic action of HD 24431. The associated neutral atomic and ionized masses are 180 M⊙ and 300 M⊙, respectively. The emission of SH 149.25-0.0 is too faint to derive the dust and gas parameters. An H I shell centred at (l, b) = (149°0', -1°30') was also identified. It correlates morphologically with the molecular gas emission. The neutral atomic and molecular masses of the shell are 1600 M⊙ and 2.6 × 104 M⊙, respectively. The open cluster NGC 1444 is probably responsible for shaping this H I structure.Facultad de Ciencias Astronómicas y GeofísicasInstituto Argentino de Radioastronomía2008-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf1080-1092http://sedici.unlp.edu.ar/handle/10915/84774enginfo:eu-repo/semantics/altIdentifier/issn/0035-8711info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2008.13117.xinfo: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:UNLP2025-09-29T11:16:11Zoai:sedici.unlp.edu.ar:10915/84774Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:11.468SEDICI (UNLP) - Universidad Nacional de La Platafalse |
dc.title.none.fl_str_mv |
Sh2-205 - I: the surrounding interstellar medium |
title |
Sh2-205 - I: the surrounding interstellar medium |
spellingShingle |
Sh2-205 - I: the surrounding interstellar medium Romero, Gisela Andrea Ciencias Astronómicas ISM: bubbles - ISM: structure Stars: individual: ALS 7793 Stars: individual: HD 24094 Stars: individual: HD 24431 |
title_short |
Sh2-205 - I: the surrounding interstellar medium |
title_full |
Sh2-205 - I: the surrounding interstellar medium |
title_fullStr |
Sh2-205 - I: the surrounding interstellar medium |
title_full_unstemmed |
Sh2-205 - I: the surrounding interstellar medium |
title_sort |
Sh2-205 - I: the surrounding interstellar medium |
dc.creator.none.fl_str_mv |
Romero, Gisela Andrea Cappa, Cristina Elisabet |
author |
Romero, Gisela Andrea |
author_facet |
Romero, Gisela Andrea Cappa, Cristina Elisabet |
author_role |
author |
author2 |
Cappa, Cristina Elisabet |
author2_role |
author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas ISM: bubbles - ISM: structure Stars: individual: ALS 7793 Stars: individual: HD 24094 Stars: individual: HD 24431 |
topic |
Ciencias Astronómicas ISM: bubbles - ISM: structure Stars: individual: ALS 7793 Stars: individual: HD 24094 Stars: individual: HD 24431 |
dc.description.none.fl_txt_mv |
We investigate the distribution of the interstellar matter in the environs of the H II region Sh2-205, based on neutral hydrogen 21-cm-line data and radio continuum images at 408 and 1420 MHz obtained from the CGPS, 12CO (J=1 →0) observations, high-resolution IRAS data (HIRES), and MSX data. Sh2-205 can be separated into three distinct optical structures: SH 149.25-0.0, SH 148.83-0.67, and LBN 148.11-0.45. The three regions are detected at both 408 and 1420 MHz. The derived spectral indices show the thermal nature of SH 148.83-0.67 and LBN 148.11-0.45. LBN 148.11-0.45 is a classical H II region surrounded by an H i shell. The associated neutral atomic and ionized masses are 65 M⊙ and 70 M⊙, respectively. Dust and molecular gas (∼6 × 104 M⊙) related to this ionized region have been found. In particular, a photodissociation region is detected at the interface between the ionized and molecular regions. If the proposed exciting star HD 24094 were an O8-O9 type star, as suggested by its near-infrared colours, its UV photon flux would be strong enough to explain the ionization of the nebula. The optical, radio continuum, and 21-cm-line data allow us to conclude that SH 148.83-0.67 is an interstellar bubble powered by the energetic action of HD 24431. The associated neutral atomic and ionized masses are 180 M⊙ and 300 M⊙, respectively. The emission of SH 149.25-0.0 is too faint to derive the dust and gas parameters. An H I shell centred at (l, b) = (149°0', -1°30') was also identified. It correlates morphologically with the molecular gas emission. The neutral atomic and molecular masses of the shell are 1600 M⊙ and 2.6 × 104 M⊙, respectively. The open cluster NGC 1444 is probably responsible for shaping this H I structure. Facultad de Ciencias Astronómicas y Geofísicas Instituto Argentino de Radioastronomía |
description |
We investigate the distribution of the interstellar matter in the environs of the H II region Sh2-205, based on neutral hydrogen 21-cm-line data and radio continuum images at 408 and 1420 MHz obtained from the CGPS, 12CO (J=1 →0) observations, high-resolution IRAS data (HIRES), and MSX data. Sh2-205 can be separated into three distinct optical structures: SH 149.25-0.0, SH 148.83-0.67, and LBN 148.11-0.45. The three regions are detected at both 408 and 1420 MHz. The derived spectral indices show the thermal nature of SH 148.83-0.67 and LBN 148.11-0.45. LBN 148.11-0.45 is a classical H II region surrounded by an H i shell. The associated neutral atomic and ionized masses are 65 M⊙ and 70 M⊙, respectively. Dust and molecular gas (∼6 × 104 M⊙) related to this ionized region have been found. In particular, a photodissociation region is detected at the interface between the ionized and molecular regions. If the proposed exciting star HD 24094 were an O8-O9 type star, as suggested by its near-infrared colours, its UV photon flux would be strong enough to explain the ionization of the nebula. The optical, radio continuum, and 21-cm-line data allow us to conclude that SH 148.83-0.67 is an interstellar bubble powered by the energetic action of HD 24431. The associated neutral atomic and ionized masses are 180 M⊙ and 300 M⊙, respectively. The emission of SH 149.25-0.0 is too faint to derive the dust and gas parameters. An H I shell centred at (l, b) = (149°0', -1°30') was also identified. It correlates morphologically with the molecular gas emission. The neutral atomic and molecular masses of the shell are 1600 M⊙ and 2.6 × 104 M⊙, respectively. The open cluster NGC 1444 is probably responsible for shaping this H I structure. |
publishDate |
2008 |
dc.date.none.fl_str_mv |
2008-07 |
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 |
format |
article |
status_str |
publishedVersion |
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http://sedici.unlp.edu.ar/handle/10915/84774 |
url |
http://sedici.unlp.edu.ar/handle/10915/84774 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/issn/0035-8711 info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2008.13117.x |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess 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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openAccess |
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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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