Physical characterization of S169: a prototypical IR bubble associated with the massive star-forming region IRAS 12326-6245
- Autores
- Duronea, Nicolás Urbano; Cichowolski, Silvina; Bronfman, Leonardo; Mendoza, E.; Finger, Ricardo; 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.
Instituto de Astrofísica de La Plata - Materia
-
Ciencias Astronómicas
Astronomía
ISM: molecules
ISM: IR dust bubbles
ISM: individual object: S169
ISM:individual object: IRAS 12326-6245 - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by/4.0/
- Repositorio
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/124993
Ver los metadatos del registro completo
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Physical characterization of S169: a prototypical IR bubble associated with the massive star-forming region IRAS 12326-6245Duronea, Nicolás UrbanoCichowolski, SilvinaBronfman, LeonardoMendoza, E.Finger, RicardoSuad, Laura AndreaCorti, Mariela AlejandraReynoso, Estela MartaCiencias AstronómicasAstronomíaISM: moleculesISM: IR dust bubblesISM: individual object: S169ISM:individual object: IRAS 12326-6245<i>Aims</i>. 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),<sup>13</sup>CO(2-1), C<sup>18</sup>O(2-1), HCN(3-2), and HCO<sup>+</sup> (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, <i>Herschel</i>, 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. <i>Results</i>. 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<sup>−1</sup> (component A), −25 km s<sup>−1</sup> (component B), and −17 km s<sup>−1</sup> (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 H<sub>2</sub> column density up to 8×10<sup>23</sup> cm<sup>−2</sup> . An LTE analysis of the high density tracer lines HCO<sup>+</sup> (3-2) and HCN(3-2) on this source, assuming 50 and 150 K, respectively, indicates column densities of N(HCO<sup>+</sup>) = (5.2 ± 0.1) × 10<sup>13</sup> cm<sup>−2</sup> and N(HCN) = (1.9 ± 0.5) × 10<sup>14</sup> cm<sup>−2</sup>. 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<sup>−1</sup>. 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.Instituto de Astrofísica de La Plata2021-02info: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/10915/124993enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/issn/1432-0746info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202039074info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/4.0/Creative Commons Attribution 4.0 International (CC BY 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:29:54Zoai:sedici.unlp.edu.ar:10915/124993Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:29:54.518SEDICI (UNLP) - Universidad Nacional de La Platafalse |
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, Nicolás Urbano Ciencias Astronómicas Astronomía ISM: molecules ISM: IR dust bubbles ISM: individual object: S169 ISM:individual object: IRAS 12326-6245 |
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, Nicolás Urbano Cichowolski, Silvina Bronfman, Leonardo Mendoza, E. Finger, Ricardo Suad, Laura Andrea Corti, Mariela Alejandra Reynoso, Estela Marta |
author |
Duronea, Nicolás Urbano |
author_facet |
Duronea, Nicolás Urbano Cichowolski, Silvina Bronfman, Leonardo Mendoza, E. Finger, Ricardo Suad, Laura Andrea Corti, Mariela Alejandra Reynoso, Estela Marta |
author_role |
author |
author2 |
Cichowolski, Silvina Bronfman, Leonardo Mendoza, E. Finger, Ricardo Suad, Laura Andrea Corti, Mariela Alejandra Reynoso, Estela Marta |
author2_role |
author author author author author author author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas Astronomía ISM: molecules ISM: IR dust bubbles ISM: individual object: S169 ISM:individual object: IRAS 12326-6245 |
topic |
Ciencias Astronómicas Astronomía ISM: molecules ISM: IR dust bubbles ISM: individual object: S169 ISM:individual object: IRAS 12326-6245 |
dc.description.none.fl_txt_mv |
<i>Aims</i>. 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),<sup>13</sup>CO(2-1), C<sup>18</sup>O(2-1), HCN(3-2), and HCO<sup>+</sup> (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, <i>Herschel</i>, 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. <i>Results</i>. 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<sup>−1</sup> (component A), −25 km s<sup>−1</sup> (component B), and −17 km s<sup>−1</sup> (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 H<sub>2</sub> column density up to 8×10<sup>23</sup> cm<sup>−2</sup> . An LTE analysis of the high density tracer lines HCO<sup>+</sup> (3-2) and HCN(3-2) on this source, assuming 50 and 150 K, respectively, indicates column densities of N(HCO<sup>+</sup>) = (5.2 ± 0.1) × 10<sup>13</sup> cm<sup>−2</sup> and N(HCN) = (1.9 ± 0.5) × 10<sup>14</sup> cm<sup>−2</sup>. 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<sup>−1</sup>. 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. Instituto de Astrofísica de La Plata |
description |
<i>Aims</i>. 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),<sup>13</sup>CO(2-1), C<sup>18</sup>O(2-1), HCN(3-2), and HCO<sup>+</sup> (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, <i>Herschel</i>, 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. <i>Results</i>. 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<sup>−1</sup> (component A), −25 km s<sup>−1</sup> (component B), and −17 km s<sup>−1</sup> (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 H<sub>2</sub> column density up to 8×10<sup>23</sup> cm<sup>−2</sup> . An LTE analysis of the high density tracer lines HCO<sup>+</sup> (3-2) and HCN(3-2) on this source, assuming 50 and 150 K, respectively, indicates column densities of N(HCO<sup>+</sup>) = (5.2 ± 0.1) × 10<sup>13</sup> cm<sup>−2</sup> and N(HCN) = (1.9 ± 0.5) × 10<sup>14</sup> cm<sup>−2</sup>. 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<sup>−1</sup>. 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 |
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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article |
status_str |
publishedVersion |
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http://sedici.unlp.edu.ar/handle/10915/124993 |
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http://sedici.unlp.edu.ar/handle/10915/124993 |
dc.language.none.fl_str_mv |
eng |
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eng |
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info:eu-repo/semantics/altIdentifier/issn/0004-6361 info:eu-repo/semantics/altIdentifier/issn/1432-0746 info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202039074 |
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info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/4.0/ Creative Commons Attribution 4.0 International (CC BY 4.0) |
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openAccess |
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http://creativecommons.org/licenses/by/4.0/ Creative Commons Attribution 4.0 International (CC BY 4.0) |
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