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
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/84774

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oai_identifier_str oai:sedici.unlp.edu.ar:10915/84774
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling 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
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info:ar-repo/semantics/articulo
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status_str publishedVersion
dc.identifier.none.fl_str_mv 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
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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)
eu_rights_str_mv openAccess
rights_invalid_str_mv 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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1080-1092
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instname:Universidad Nacional de La Plata
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