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
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/124993

id SEDICI_2dac27663c113266cf411dea3edb7859
oai_identifier_str oai:sedici.unlp.edu.ar:10915/124993
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling 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
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format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://sedici.unlp.edu.ar/handle/10915/124993
url http://sedici.unlp.edu.ar/handle/10915/124993
dc.language.none.fl_str_mv eng
language eng
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info:eu-repo/semantics/altIdentifier/issn/1432-0746
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202039074
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by/4.0/
Creative Commons Attribution 4.0 International (CC BY 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by/4.0/
Creative Commons Attribution 4.0 International (CC BY 4.0)
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
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reponame_str SEDICI (UNLP)
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repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
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