NGC 3503 and its molecular environment
- Autores
- Duronea, Nicolás Urbano; Vasquez, Javier; Cappa, Cristina Elisabet; Corti, Mariela Alejandra; Arnal, Edmundo Marcelo
- Año de publicación
- 2012
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Aims. We present a study of the molecular gas and interstellar dust distribution in the environs of the Hiiπ region NGC 3503 associated with the open cluster Pis 17 with the aim of investigating the spatial distribution of the molecular gas linked to the nebula and achieving a better understanding of the interaction of the nebula and Pis 17 with their molecular environment. Methods. We based our study on 12CO(1-0) observations of a region of ∼0°6 in size obtained with the 4-m NANTEN telescope, unpublished radio continuum data at 4800 and 8640 MHz obtained with the ATCA telescope, radio continuum data at 843 MHz obtained from SUMSS, and available IRAS, MSX, IRAC-GLIMPSE, and MIPSGAL images. Results. We found a molecular cloud (Component 1) having a mean velocity of -24.7 km s -1 ,compatible with the velocity of the ionized gas, which is associated with the nebula and its surroundings. Adopting a distance of 2.9 ± 0.4 kpc, the total molecular mass yields (7.6 ± 2.1) × 10 3M⊙ and density yields 400 ± 240 cm -3. The radio continuum data confirm the existence of an electron density gradient in NGC 3503. The IR emission shows a PDR bordering the higher density regions of the nebula. The spatial distribution of the CO emission shows that the nebula coincides with a molecular clump, and the strongest CO emission peak is located close to the higher electron density region. The more negative velocities of the molecular gas (about -27 km s -1), are coincident with NGC 3503. Candidate young stellar objects (YSOs) were detected toward the Hii region, suggesting that embedded star formation may be occurring in the neighborhood of the nebula. The clear electron density gradient, along with the spatial distribution of the molecular gas and PAHs in the region indicates that NGC 3503 is a blister-type Hii region that has probably undergone a champagne phase.
Facultad de Ciencias Astronómicas y Geofísicas - Materia
-
Ciencias Astronómicas
HII regions
ISM: clouds
ISM: kinematics and dynamics
ISM: molecules
Photon-dominated region (PDR)
Radio continuum: ISM - 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:10915/84622
Ver los metadatos del registro completo
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NGC 3503 and its molecular environmentDuronea, Nicolás UrbanoVasquez, JavierCappa, Cristina ElisabetCorti, Mariela AlejandraArnal, Edmundo MarceloCiencias AstronómicasHII regionsISM: cloudsISM: kinematics and dynamicsISM: moleculesPhoton-dominated region (PDR)Radio continuum: ISM<b>Aims.</b> We present a study of the molecular gas and interstellar dust distribution in the environs of the Hiiπ region NGC 3503 associated with the open cluster Pis 17 with the aim of investigating the spatial distribution of the molecular gas linked to the nebula and achieving a better understanding of the interaction of the nebula and Pis 17 with their molecular environment. <b>Methods.</b> We based our study on 12CO(1-0) observations of a region of ∼0°6 in size obtained with the 4-m NANTEN telescope, unpublished radio continuum data at 4800 and 8640 MHz obtained with the ATCA telescope, radio continuum data at 843 MHz obtained from SUMSS, and available IRAS, MSX, IRAC-GLIMPSE, and MIPSGAL images. <b>Results.</b> We found a molecular cloud (Component 1) having a mean velocity of -24.7 km s -1 ,compatible with the velocity of the ionized gas, which is associated with the nebula and its surroundings. Adopting a distance of 2.9 ± 0.4 kpc, the total molecular mass yields (7.6 ± 2.1) × 10 3M⊙ and density yields 400 ± 240 cm -3. The radio continuum data confirm the existence of an electron density gradient in NGC 3503. The IR emission shows a PDR bordering the higher density regions of the nebula. The spatial distribution of the CO emission shows that the nebula coincides with a molecular clump, and the strongest CO emission peak is located close to the higher electron density region. The more negative velocities of the molecular gas (about -27 km s -1), are coincident with NGC 3503. Candidate young stellar objects (YSOs) were detected toward the Hii region, suggesting that embedded star formation may be occurring in the neighborhood of the nebula. The clear electron density gradient, along with the spatial distribution of the molecular gas and PAHs in the region indicates that NGC 3503 is a blister-type Hii region that has probably undergone a champagne phase.Facultad de Ciencias Astronómicas y Geofísicas2012-01-12info: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/10915/84622enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201117958info: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:10915/84622Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:05.534SEDICI (UNLP) - Universidad Nacional de La Platafalse |
dc.title.none.fl_str_mv |
NGC 3503 and its molecular environment |
title |
NGC 3503 and its molecular environment |
spellingShingle |
NGC 3503 and its molecular environment Duronea, Nicolás Urbano Ciencias Astronómicas HII regions ISM: clouds ISM: kinematics and dynamics ISM: molecules Photon-dominated region (PDR) Radio continuum: ISM |
title_short |
NGC 3503 and its molecular environment |
title_full |
NGC 3503 and its molecular environment |
title_fullStr |
NGC 3503 and its molecular environment |
title_full_unstemmed |
NGC 3503 and its molecular environment |
title_sort |
NGC 3503 and its molecular environment |
dc.creator.none.fl_str_mv |
Duronea, Nicolás Urbano Vasquez, Javier Cappa, Cristina Elisabet Corti, Mariela Alejandra Arnal, Edmundo Marcelo |
author |
Duronea, Nicolás Urbano |
author_facet |
Duronea, Nicolás Urbano Vasquez, Javier Cappa, Cristina Elisabet Corti, Mariela Alejandra Arnal, Edmundo Marcelo |
author_role |
author |
author2 |
Vasquez, Javier Cappa, Cristina Elisabet Corti, Mariela Alejandra Arnal, Edmundo Marcelo |
author2_role |
author author author author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas HII regions ISM: clouds ISM: kinematics and dynamics ISM: molecules Photon-dominated region (PDR) Radio continuum: ISM |
topic |
Ciencias Astronómicas HII regions ISM: clouds ISM: kinematics and dynamics ISM: molecules Photon-dominated region (PDR) Radio continuum: ISM |
dc.description.none.fl_txt_mv |
<b>Aims.</b> We present a study of the molecular gas and interstellar dust distribution in the environs of the Hiiπ region NGC 3503 associated with the open cluster Pis 17 with the aim of investigating the spatial distribution of the molecular gas linked to the nebula and achieving a better understanding of the interaction of the nebula and Pis 17 with their molecular environment. <b>Methods.</b> We based our study on 12CO(1-0) observations of a region of ∼0°6 in size obtained with the 4-m NANTEN telescope, unpublished radio continuum data at 4800 and 8640 MHz obtained with the ATCA telescope, radio continuum data at 843 MHz obtained from SUMSS, and available IRAS, MSX, IRAC-GLIMPSE, and MIPSGAL images. <b>Results.</b> We found a molecular cloud (Component 1) having a mean velocity of -24.7 km s -1 ,compatible with the velocity of the ionized gas, which is associated with the nebula and its surroundings. Adopting a distance of 2.9 ± 0.4 kpc, the total molecular mass yields (7.6 ± 2.1) × 10 3M⊙ and density yields 400 ± 240 cm -3. The radio continuum data confirm the existence of an electron density gradient in NGC 3503. The IR emission shows a PDR bordering the higher density regions of the nebula. The spatial distribution of the CO emission shows that the nebula coincides with a molecular clump, and the strongest CO emission peak is located close to the higher electron density region. The more negative velocities of the molecular gas (about -27 km s -1), are coincident with NGC 3503. Candidate young stellar objects (YSOs) were detected toward the Hii region, suggesting that embedded star formation may be occurring in the neighborhood of the nebula. The clear electron density gradient, along with the spatial distribution of the molecular gas and PAHs in the region indicates that NGC 3503 is a blister-type Hii region that has probably undergone a champagne phase. Facultad de Ciencias Astronómicas y Geofísicas |
description |
<b>Aims.</b> We present a study of the molecular gas and interstellar dust distribution in the environs of the Hiiπ region NGC 3503 associated with the open cluster Pis 17 with the aim of investigating the spatial distribution of the molecular gas linked to the nebula and achieving a better understanding of the interaction of the nebula and Pis 17 with their molecular environment. <b>Methods.</b> We based our study on 12CO(1-0) observations of a region of ∼0°6 in size obtained with the 4-m NANTEN telescope, unpublished radio continuum data at 4800 and 8640 MHz obtained with the ATCA telescope, radio continuum data at 843 MHz obtained from SUMSS, and available IRAS, MSX, IRAC-GLIMPSE, and MIPSGAL images. <b>Results.</b> We found a molecular cloud (Component 1) having a mean velocity of -24.7 km s -1 ,compatible with the velocity of the ionized gas, which is associated with the nebula and its surroundings. Adopting a distance of 2.9 ± 0.4 kpc, the total molecular mass yields (7.6 ± 2.1) × 10 3M⊙ and density yields 400 ± 240 cm -3. The radio continuum data confirm the existence of an electron density gradient in NGC 3503. The IR emission shows a PDR bordering the higher density regions of the nebula. The spatial distribution of the CO emission shows that the nebula coincides with a molecular clump, and the strongest CO emission peak is located close to the higher electron density region. The more negative velocities of the molecular gas (about -27 km s -1), are coincident with NGC 3503. Candidate young stellar objects (YSOs) were detected toward the Hii region, suggesting that embedded star formation may be occurring in the neighborhood of the nebula. The clear electron density gradient, along with the spatial distribution of the molecular gas and PAHs in the region indicates that NGC 3503 is a blister-type Hii region that has probably undergone a champagne phase. |
publishDate |
2012 |
dc.date.none.fl_str_mv |
2012-01-12 |
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 |
dc.identifier.none.fl_str_mv |
http://sedici.unlp.edu.ar/handle/10915/84622 |
url |
http://sedici.unlp.edu.ar/handle/10915/84622 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/issn/0004-6361 info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201117958 |
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) |
dc.format.none.fl_str_mv |
application/pdf |
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