Molecular gas associated with IRAS 10361-5830
- Autores
- Vazzano, María Mercedes; Cappa, Cristina Elisabet; Vasquez, Javier; Rubio, Mónica; Romero, Gisela Andrea
- Año de publicación
- 2014
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Aims. We analyze the distribution of the molecular gas and dust in the molecular clump linked to IRAS 10361-5830, located in the environs of the bubble-shaped HII region Gum 31 in the Carina region, with the aim of determining the main parameters of the associated material and of investigating the evolutionary state of the young stellar objects identified there. Methods. Using the APEX telescope, we mapped the molecular emission in the J = 3-2 transition of three CO isotopologues, 12CO, 13CO and C18O, over a 1. 5 × 1. 5 region around the IRAS position. We also observed the high-density tracers CS and HCO+ toward the source. The cold-dust distribution was analyzed using submillimeter continuum data at 870 μm obtained with the APEX telescope. Complementary IR and radio data at different wavelengths were used to complete the study of the interstellar medium. Results. The molecular gas distribution reveals a cavity and a shell-like structure of ~0.32 pc in radius centered at the position of the IRAS source, with some young stellar objects projected onto the cavity. The total molecular mass in the shell and the mean H2 volume density are ~40 M and ~(1-2) × 103 cm-3. The cold-dust counterpart of the molecular shell has been detected in the far-IR at 870 μm and in Herschel data at 350 μm. Weak extended emission at 24 μm from warm dust is projected onto the cavity, as well as weak radio continuum emission. Conclusions. A comparison of the distribution of cold and warm dust, and molecular and ionized gas allows us to conclude that a compact HII region has developed in the molecular clump, indicating that this is an area of recent massive star formation. Probable exciting sources capable of creating the compact HII region are investigated. The 2MASS source 10380461-5846233 (MSX G286.3773-00.2563) seems to be responsible for the formation of the HII region..
Facultad de Ciencias Astronómicas y Geofísicas
Instituto Argentino de Radioastronomía - Materia
-
Ciencias Astronómicas
HII regions
ISM: individual objects: IRAS 10361-5830
ISM: molecules
Stars: protostars - 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:10915/85008
Ver los metadatos del registro completo
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Molecular gas associated with IRAS 10361-5830Vazzano, María MercedesCappa, Cristina ElisabetVasquez, JavierRubio, MónicaRomero, Gisela AndreaCiencias AstronómicasHII regionsISM: individual objects: IRAS 10361-5830ISM: moleculesStars: protostarsAims. We analyze the distribution of the molecular gas and dust in the molecular clump linked to IRAS 10361-5830, located in the environs of the bubble-shaped HII region Gum 31 in the Carina region, with the aim of determining the main parameters of the associated material and of investigating the evolutionary state of the young stellar objects identified there. Methods. Using the APEX telescope, we mapped the molecular emission in the J = 3-2 transition of three CO isotopologues, <SUP>12</SUP>CO, <SUP>13</SUP>CO and C<SUP>18</SUP>O, over a 1. 5 × 1. 5 region around the IRAS position. We also observed the high-density tracers CS and HCO<SUP>+</SUP> toward the source. The cold-dust distribution was analyzed using submillimeter continuum data at 870 μm obtained with the APEX telescope. Complementary IR and radio data at different wavelengths were used to complete the study of the interstellar medium. Results. The molecular gas distribution reveals a cavity and a shell-like structure of ~0.32 pc in radius centered at the position of the IRAS source, with some young stellar objects projected onto the cavity. The total molecular mass in the shell and the mean H<SUB>2</SUB> volume density are ~40 M and ~(1-2) × 10<SUP>3</SUP> cm<SUP>-3</SUP>. The cold-dust counterpart of the molecular shell has been detected in the far-IR at 870 μm and in <i>Herschel</i> data at 350 μm. Weak extended emission at 24 μm from warm dust is projected onto the cavity, as well as weak radio continuum emission. Conclusions. A comparison of the distribution of cold and warm dust, and molecular and ionized gas allows us to conclude that a compact HII region has developed in the molecular clump, indicating that this is an area of recent massive star formation. Probable exciting sources capable of creating the compact HII region are investigated. The 2MASS source 10380461-5846233 (MSX G286.3773-00.2563) seems to be responsible for the formation of the HII region..Facultad de Ciencias Astronómicas y GeofísicasInstituto Argentino de Radioastronomía2014info: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/10915/85008enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201423369info: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:UNLP2025-09-29T11:16:20Zoai:sedici.unlp.edu.ar:10915/85008Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:21.165SEDICI (UNLP) - Universidad Nacional de La Platafalse |
dc.title.none.fl_str_mv |
Molecular gas associated with IRAS 10361-5830 |
title |
Molecular gas associated with IRAS 10361-5830 |
spellingShingle |
Molecular gas associated with IRAS 10361-5830 Vazzano, María Mercedes Ciencias Astronómicas HII regions ISM: individual objects: IRAS 10361-5830 ISM: molecules Stars: protostars |
title_short |
Molecular gas associated with IRAS 10361-5830 |
title_full |
Molecular gas associated with IRAS 10361-5830 |
title_fullStr |
Molecular gas associated with IRAS 10361-5830 |
title_full_unstemmed |
Molecular gas associated with IRAS 10361-5830 |
title_sort |
Molecular gas associated with IRAS 10361-5830 |
dc.creator.none.fl_str_mv |
Vazzano, María Mercedes Cappa, Cristina Elisabet Vasquez, Javier Rubio, Mónica Romero, Gisela Andrea |
author |
Vazzano, María Mercedes |
author_facet |
Vazzano, María Mercedes Cappa, Cristina Elisabet Vasquez, Javier Rubio, Mónica Romero, Gisela Andrea |
author_role |
author |
author2 |
Cappa, Cristina Elisabet Vasquez, Javier Rubio, Mónica Romero, Gisela Andrea |
author2_role |
author author author author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas HII regions ISM: individual objects: IRAS 10361-5830 ISM: molecules Stars: protostars |
topic |
Ciencias Astronómicas HII regions ISM: individual objects: IRAS 10361-5830 ISM: molecules Stars: protostars |
dc.description.none.fl_txt_mv |
Aims. We analyze the distribution of the molecular gas and dust in the molecular clump linked to IRAS 10361-5830, located in the environs of the bubble-shaped HII region Gum 31 in the Carina region, with the aim of determining the main parameters of the associated material and of investigating the evolutionary state of the young stellar objects identified there. Methods. Using the APEX telescope, we mapped the molecular emission in the J = 3-2 transition of three CO isotopologues, <SUP>12</SUP>CO, <SUP>13</SUP>CO and C<SUP>18</SUP>O, over a 1. 5 × 1. 5 region around the IRAS position. We also observed the high-density tracers CS and HCO<SUP>+</SUP> toward the source. The cold-dust distribution was analyzed using submillimeter continuum data at 870 μm obtained with the APEX telescope. Complementary IR and radio data at different wavelengths were used to complete the study of the interstellar medium. Results. The molecular gas distribution reveals a cavity and a shell-like structure of ~0.32 pc in radius centered at the position of the IRAS source, with some young stellar objects projected onto the cavity. The total molecular mass in the shell and the mean H<SUB>2</SUB> volume density are ~40 M and ~(1-2) × 10<SUP>3</SUP> cm<SUP>-3</SUP>. The cold-dust counterpart of the molecular shell has been detected in the far-IR at 870 μm and in <i>Herschel</i> data at 350 μm. Weak extended emission at 24 μm from warm dust is projected onto the cavity, as well as weak radio continuum emission. Conclusions. A comparison of the distribution of cold and warm dust, and molecular and ionized gas allows us to conclude that a compact HII region has developed in the molecular clump, indicating that this is an area of recent massive star formation. Probable exciting sources capable of creating the compact HII region are investigated. The 2MASS source 10380461-5846233 (MSX G286.3773-00.2563) seems to be responsible for the formation of the HII region.. Facultad de Ciencias Astronómicas y Geofísicas Instituto Argentino de Radioastronomía |
description |
Aims. We analyze the distribution of the molecular gas and dust in the molecular clump linked to IRAS 10361-5830, located in the environs of the bubble-shaped HII region Gum 31 in the Carina region, with the aim of determining the main parameters of the associated material and of investigating the evolutionary state of the young stellar objects identified there. Methods. Using the APEX telescope, we mapped the molecular emission in the J = 3-2 transition of three CO isotopologues, <SUP>12</SUP>CO, <SUP>13</SUP>CO and C<SUP>18</SUP>O, over a 1. 5 × 1. 5 region around the IRAS position. We also observed the high-density tracers CS and HCO<SUP>+</SUP> toward the source. The cold-dust distribution was analyzed using submillimeter continuum data at 870 μm obtained with the APEX telescope. Complementary IR and radio data at different wavelengths were used to complete the study of the interstellar medium. Results. The molecular gas distribution reveals a cavity and a shell-like structure of ~0.32 pc in radius centered at the position of the IRAS source, with some young stellar objects projected onto the cavity. The total molecular mass in the shell and the mean H<SUB>2</SUB> volume density are ~40 M and ~(1-2) × 10<SUP>3</SUP> cm<SUP>-3</SUP>. The cold-dust counterpart of the molecular shell has been detected in the far-IR at 870 μm and in <i>Herschel</i> data at 350 μm. Weak extended emission at 24 μm from warm dust is projected onto the cavity, as well as weak radio continuum emission. Conclusions. A comparison of the distribution of cold and warm dust, and molecular and ionized gas allows us to conclude that a compact HII region has developed in the molecular clump, indicating that this is an area of recent massive star formation. Probable exciting sources capable of creating the compact HII region are investigated. The 2MASS source 10380461-5846233 (MSX G286.3773-00.2563) seems to be responsible for the formation of the HII region.. |
publishDate |
2014 |
dc.date.none.fl_str_mv |
2014 |
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/10915/85008 |
url |
http://sedici.unlp.edu.ar/handle/10915/85008 |
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/10.1051/0004-6361/201423369 |
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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) |
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openAccess |
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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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