Physical characterization of S169: a prototypical IR bubble associated with the massive star-forming region IRAS 12326-6245
- Autores
- Duronea, Nicolas Urbano; Cichowolski, Silvina; Bronfman, L.; Mendoza, E.; Finger, R.; Suad, Laura Andrea; Corti, Mariela Alejandra; Reynoso, Estela Marta
- Año de publicación
- 2021
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Aims. With the aim of studying the physical properties of Galactic IR bubbles and to explore their impact in massive star formation, we present a study of the IR bubble S169, associated with the massive star forming region IRAS 12326-6245. Methods. We used CO(2-1),13CO(2-1), C18O(2-1), HCN(3-2), and HCO+ (3-2) line data obtained with the APEX telescope using the on-the-fly full sampling technique to study the properties of the molecular gas in the nebula and the IRAS source . To analyze the properties and distribution of the dust, we made use of images obtained from the IRAC-GLIMPSE, Herschel, and ATLASGAL archives. The properties of the ionized gas in the nebula were studied using radio continuum and Hα images obtained from the SUMSS survey and SuperCOSMOS database, respectively. In our search for stellar and protostellar objects in the region, we used point source calalogs obtained from the MSX, WISE, GLIMPSE, 2MASS, AAVSO, ASCC-2.5V3, and GAIA databases. Results. The new APEX observations allowed us to identify three molecular components, each one associated with different regions of the nebula, namely: at −39 km s−1 (component A), −25 km s−1 (component B), and −17 km s−1 (component C). Component A is shown to be the most dense and clumpy. Six molecular condensations (MC1 to MC6) were identified in this component, with MC3 (the densest and more massive one) being the molecular counterpart of IRAS 12326-6245. For this source, we estimated an H2 column density up to 8×1023 cm−2 . An LTE analysis of the high density tracer lines HCO+ (3-2) and HCN(3-2) on this source, assuming 50 and 150 K, respectively, indicates column densities of N(HCO+ ) = (5.2 ± 0.1) × 1013 cm−2 and N(HCN) = (1.9 ± 0.5) × 1014 cm−2 . To explain the morphology and velocity of components A, B, and C , we propose a simple model consisting of a partially complete semisphere-like structure expanding at ∼ 12 km s−1 . The introduction of this model has led to a discussion about the distance to both S169 and IRAS 12326-6245, which was estimated to be ∼ 2 kpc. Several candidate YSOs were identified, projected mostly onto the molecular condensations MC3, MC4, and MC5, which indicates that the star-formation process is very active at the borders of the nebula. A comparison between observable and modeled parameters was not enough to discern whether the collect-and-collapse mechanism is acting at the edge of S169. However, other processes such as radiative-driven implosion or even a combination of both mechanisms, namely, collect-and-collapse and radiative-driven implosion, could be acting simultaneously in the region.
Fil: Duronea, Nicolas Urbano. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Cichowolski, Silvina. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Bronfman, L.. Universidad de Chile; Chile
Fil: Mendoza, E.. Universidade Federal do Rio de Janeiro; Brasil
Fil: Finger, R.. Universidad de Chile; Chile
Fil: Suad, Laura Andrea. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina
Fil: Corti, Mariela Alejandra. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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: Reynoso, Estela Marta. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina - Materia
-
HII REGIONS
ISM: BUBBLES
ISM: KINEMATICS AND DYNAMICS
ISM: MOLECULES - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/183101
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Physical characterization of S169: a prototypical IR bubble associated with the massive star-forming region IRAS 12326-6245Duronea, Nicolas UrbanoCichowolski, SilvinaBronfman, L.Mendoza, E.Finger, R.Suad, Laura AndreaCorti, Mariela AlejandraReynoso, Estela MartaHII REGIONSISM: BUBBLESISM: KINEMATICS AND DYNAMICSISM: MOLECULEShttps://purl.org/becyt/ford/1.7https://purl.org/becyt/ford/1Aims. With the aim of studying the physical properties of Galactic IR bubbles and to explore their impact in massive star formation, we present a study of the IR bubble S169, associated with the massive star forming region IRAS 12326-6245. Methods. We used CO(2-1),13CO(2-1), C18O(2-1), HCN(3-2), and HCO+ (3-2) line data obtained with the APEX telescope using the on-the-fly full sampling technique to study the properties of the molecular gas in the nebula and the IRAS source . To analyze the properties and distribution of the dust, we made use of images obtained from the IRAC-GLIMPSE, Herschel, and ATLASGAL archives. The properties of the ionized gas in the nebula were studied using radio continuum and Hα images obtained from the SUMSS survey and SuperCOSMOS database, respectively. In our search for stellar and protostellar objects in the region, we used point source calalogs obtained from the MSX, WISE, GLIMPSE, 2MASS, AAVSO, ASCC-2.5V3, and GAIA databases. Results. The new APEX observations allowed us to identify three molecular components, each one associated with different regions of the nebula, namely: at −39 km s−1 (component A), −25 km s−1 (component B), and −17 km s−1 (component C). Component A is shown to be the most dense and clumpy. Six molecular condensations (MC1 to MC6) were identified in this component, with MC3 (the densest and more massive one) being the molecular counterpart of IRAS 12326-6245. For this source, we estimated an H2 column density up to 8×1023 cm−2 . An LTE analysis of the high density tracer lines HCO+ (3-2) and HCN(3-2) on this source, assuming 50 and 150 K, respectively, indicates column densities of N(HCO+ ) = (5.2 ± 0.1) × 1013 cm−2 and N(HCN) = (1.9 ± 0.5) × 1014 cm−2 . To explain the morphology and velocity of components A, B, and C , we propose a simple model consisting of a partially complete semisphere-like structure expanding at ∼ 12 km s−1 . The introduction of this model has led to a discussion about the distance to both S169 and IRAS 12326-6245, which was estimated to be ∼ 2 kpc. Several candidate YSOs were identified, projected mostly onto the molecular condensations MC3, MC4, and MC5, which indicates that the star-formation process is very active at the borders of the nebula. A comparison between observable and modeled parameters was not enough to discern whether the collect-and-collapse mechanism is acting at the edge of S169. However, other processes such as radiative-driven implosion or even a combination of both mechanisms, namely, collect-and-collapse and radiative-driven implosion, could be acting simultaneously in the region.Fil: Duronea, Nicolas Urbano. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Cichowolski, Silvina. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Bronfman, L.. Universidad de Chile; ChileFil: Mendoza, E.. Universidade Federal do Rio de Janeiro; BrasilFil: Finger, R.. Universidad de Chile; ChileFil: Suad, Laura Andrea. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Corti, Mariela Alejandra. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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: Reynoso, Estela Marta. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaEDP Sciences2021-02-15info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/183101Duronea, Nicolas Urbano; Cichowolski, Silvina; Bronfman, L.; Mendoza, E.; Finger, R.; et al.; Physical characterization of S169: a prototypical IR bubble associated with the massive star-forming region IRAS 12326-6245; EDP Sciences; Astronomy and Astrophysics; 646; 15-2-2021; 1-180004-63611432-0746CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2021/02/aa39074-20/aa39074-20.htmlinfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202039074info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/2012.06328info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:28:26Zoai:ri.conicet.gov.ar:11336/183101instacron: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:34982025-09-29 10:28:26.7CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Physical characterization of S169: a prototypical IR bubble associated with the massive star-forming region IRAS 12326-6245 |
title |
Physical characterization of S169: a prototypical IR bubble associated with the massive star-forming region IRAS 12326-6245 |
spellingShingle |
Physical characterization of S169: a prototypical IR bubble associated with the massive star-forming region IRAS 12326-6245 Duronea, Nicolas Urbano HII REGIONS ISM: BUBBLES ISM: KINEMATICS AND DYNAMICS ISM: MOLECULES |
title_short |
Physical characterization of S169: a prototypical IR bubble associated with the massive star-forming region IRAS 12326-6245 |
title_full |
Physical characterization of S169: a prototypical IR bubble associated with the massive star-forming region IRAS 12326-6245 |
title_fullStr |
Physical characterization of S169: a prototypical IR bubble associated with the massive star-forming region IRAS 12326-6245 |
title_full_unstemmed |
Physical characterization of S169: a prototypical IR bubble associated with the massive star-forming region IRAS 12326-6245 |
title_sort |
Physical characterization of S169: a prototypical IR bubble associated with the massive star-forming region IRAS 12326-6245 |
dc.creator.none.fl_str_mv |
Duronea, Nicolas Urbano Cichowolski, Silvina Bronfman, L. Mendoza, E. Finger, R. Suad, Laura Andrea Corti, Mariela Alejandra Reynoso, Estela Marta |
author |
Duronea, Nicolas Urbano |
author_facet |
Duronea, Nicolas Urbano Cichowolski, Silvina Bronfman, L. Mendoza, E. Finger, R. Suad, Laura Andrea Corti, Mariela Alejandra Reynoso, Estela Marta |
author_role |
author |
author2 |
Cichowolski, Silvina Bronfman, L. Mendoza, E. Finger, R. Suad, Laura Andrea Corti, Mariela Alejandra Reynoso, Estela Marta |
author2_role |
author author author author author author author |
dc.subject.none.fl_str_mv |
HII REGIONS ISM: BUBBLES ISM: KINEMATICS AND DYNAMICS ISM: MOLECULES |
topic |
HII REGIONS ISM: BUBBLES ISM: KINEMATICS AND DYNAMICS ISM: MOLECULES |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.7 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
Aims. With the aim of studying the physical properties of Galactic IR bubbles and to explore their impact in massive star formation, we present a study of the IR bubble S169, associated with the massive star forming region IRAS 12326-6245. Methods. We used CO(2-1),13CO(2-1), C18O(2-1), HCN(3-2), and HCO+ (3-2) line data obtained with the APEX telescope using the on-the-fly full sampling technique to study the properties of the molecular gas in the nebula and the IRAS source . To analyze the properties and distribution of the dust, we made use of images obtained from the IRAC-GLIMPSE, Herschel, and ATLASGAL archives. The properties of the ionized gas in the nebula were studied using radio continuum and Hα images obtained from the SUMSS survey and SuperCOSMOS database, respectively. In our search for stellar and protostellar objects in the region, we used point source calalogs obtained from the MSX, WISE, GLIMPSE, 2MASS, AAVSO, ASCC-2.5V3, and GAIA databases. Results. The new APEX observations allowed us to identify three molecular components, each one associated with different regions of the nebula, namely: at −39 km s−1 (component A), −25 km s−1 (component B), and −17 km s−1 (component C). Component A is shown to be the most dense and clumpy. Six molecular condensations (MC1 to MC6) were identified in this component, with MC3 (the densest and more massive one) being the molecular counterpart of IRAS 12326-6245. For this source, we estimated an H2 column density up to 8×1023 cm−2 . An LTE analysis of the high density tracer lines HCO+ (3-2) and HCN(3-2) on this source, assuming 50 and 150 K, respectively, indicates column densities of N(HCO+ ) = (5.2 ± 0.1) × 1013 cm−2 and N(HCN) = (1.9 ± 0.5) × 1014 cm−2 . To explain the morphology and velocity of components A, B, and C , we propose a simple model consisting of a partially complete semisphere-like structure expanding at ∼ 12 km s−1 . The introduction of this model has led to a discussion about the distance to both S169 and IRAS 12326-6245, which was estimated to be ∼ 2 kpc. Several candidate YSOs were identified, projected mostly onto the molecular condensations MC3, MC4, and MC5, which indicates that the star-formation process is very active at the borders of the nebula. A comparison between observable and modeled parameters was not enough to discern whether the collect-and-collapse mechanism is acting at the edge of S169. However, other processes such as radiative-driven implosion or even a combination of both mechanisms, namely, collect-and-collapse and radiative-driven implosion, could be acting simultaneously in the region. Fil: Duronea, Nicolas Urbano. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina Fil: Cichowolski, Silvina. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Bronfman, L.. Universidad de Chile; Chile Fil: Mendoza, E.. Universidade Federal do Rio de Janeiro; Brasil Fil: Finger, R.. Universidad de Chile; Chile Fil: Suad, Laura Andrea. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Corti, Mariela Alejandra. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. 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: Reynoso, Estela Marta. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina |
description |
Aims. With the aim of studying the physical properties of Galactic IR bubbles and to explore their impact in massive star formation, we present a study of the IR bubble S169, associated with the massive star forming region IRAS 12326-6245. Methods. We used CO(2-1),13CO(2-1), C18O(2-1), HCN(3-2), and HCO+ (3-2) line data obtained with the APEX telescope using the on-the-fly full sampling technique to study the properties of the molecular gas in the nebula and the IRAS source . To analyze the properties and distribution of the dust, we made use of images obtained from the IRAC-GLIMPSE, Herschel, and ATLASGAL archives. The properties of the ionized gas in the nebula were studied using radio continuum and Hα images obtained from the SUMSS survey and SuperCOSMOS database, respectively. In our search for stellar and protostellar objects in the region, we used point source calalogs obtained from the MSX, WISE, GLIMPSE, 2MASS, AAVSO, ASCC-2.5V3, and GAIA databases. Results. The new APEX observations allowed us to identify three molecular components, each one associated with different regions of the nebula, namely: at −39 km s−1 (component A), −25 km s−1 (component B), and −17 km s−1 (component C). Component A is shown to be the most dense and clumpy. Six molecular condensations (MC1 to MC6) were identified in this component, with MC3 (the densest and more massive one) being the molecular counterpart of IRAS 12326-6245. For this source, we estimated an H2 column density up to 8×1023 cm−2 . An LTE analysis of the high density tracer lines HCO+ (3-2) and HCN(3-2) on this source, assuming 50 and 150 K, respectively, indicates column densities of N(HCO+ ) = (5.2 ± 0.1) × 1013 cm−2 and N(HCN) = (1.9 ± 0.5) × 1014 cm−2 . To explain the morphology and velocity of components A, B, and C , we propose a simple model consisting of a partially complete semisphere-like structure expanding at ∼ 12 km s−1 . The introduction of this model has led to a discussion about the distance to both S169 and IRAS 12326-6245, which was estimated to be ∼ 2 kpc. Several candidate YSOs were identified, projected mostly onto the molecular condensations MC3, MC4, and MC5, which indicates that the star-formation process is very active at the borders of the nebula. A comparison between observable and modeled parameters was not enough to discern whether the collect-and-collapse mechanism is acting at the edge of S169. However, other processes such as radiative-driven implosion or even a combination of both mechanisms, namely, collect-and-collapse and radiative-driven implosion, could be acting simultaneously in the region. |
publishDate |
2021 |
dc.date.none.fl_str_mv |
2021-02-15 |
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/11336/183101 Duronea, Nicolas Urbano; Cichowolski, Silvina; Bronfman, L.; Mendoza, E.; Finger, R.; et al.; Physical characterization of S169: a prototypical IR bubble associated with the massive star-forming region IRAS 12326-6245; EDP Sciences; Astronomy and Astrophysics; 646; 15-2-2021; 1-18 0004-6361 1432-0746 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/183101 |
identifier_str_mv |
Duronea, Nicolas Urbano; Cichowolski, Silvina; Bronfman, L.; Mendoza, E.; Finger, R.; et al.; Physical characterization of S169: a prototypical IR bubble associated with the massive star-forming region IRAS 12326-6245; EDP Sciences; Astronomy and Astrophysics; 646; 15-2-2021; 1-18 0004-6361 1432-0746 CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2021/02/aa39074-20/aa39074-20.html info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202039074 info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/2012.06328 |
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info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
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openAccess |
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https://creativecommons.org/licenses/by-nc-sa/2.5/ar/ |
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EDP Sciences |
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EDP Sciences |
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Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas |
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dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar |
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