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
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/85008

id SEDICI_5e307b6fd1997ca0512a863302933b55
oai_identifier_str oai:sedici.unlp.edu.ar:10915/85008
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling 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
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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
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)
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