A view of Large Magellanic Cloud H ii regions N159, N132, and N166 through the 345-GHz window

Autores
Paron, Sergio Ariel; Ortega, Martin Eduardo; Fariña, Cecilia; Cunningham, M.; Jones, P. A.; Rubio, M.
Año de publicación
2015
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We present results obtained towards the H II regions N159, N166, and N132 from the emission of several molecular lines in the 345 GHz window. Using Atacama Submillimetre Telescope Experiment, we mapped a 2.4 arcmin × 2.4 arcmin region towards the molecular cloud N159-W in the 13CO J = 3–2 line and observed several molecular lines at an infrared (IR) peak very close to a massive young stellar object. 12CO and 13CO J = 3–2 were observed towards two positions in N166 and one position in N132. The 13CO J = 3–2 map of the N159-W cloud shows that the molecular peak is shifted south-west compared to the peak of the IR emission. Towards the IR peak, we detected emission from HCN, HNC, HCO+, C2H J = 4–3, CS J = 7–6, and tentatively C18O J = 3–2. This is the first reported detection of these molecular lines in N159-W. The analysis of the C2H line yields more evidence supporting that the chemistry involving this molecular species in compact and/or UC H II regions in the Large Magellanic Cloud should be similar to that in Galactic ones. A non-LTE (local thermodynamic equilibrium) study of the CO emission suggests the presence of both cool and warm gas in the analysed region. The same analysis for the CS, HCO+, HCN, and HNC shows that it is very likely that their emissions arise mainly from warm gas with a density between 5 × 105 to some 106 cm−3. The obtained HCN/HNC abundance ratio greater than 1 is compatible with warm gas and with an star-forming scenario. From the analysis of the molecular lines observed towards N132 and N166, we propose that both regions should have similar physical conditions, with densities of about 103 cm−3.
Fil: Paron, Sergio Ariel. 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
Fil: Ortega, Martin Eduardo. 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
Fil: Fariña, Cecilia. Grupo de Telescopios Isaac Newton; España. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Cunningham, M.. University Of New South Wales; Australia
Fil: Jones, P. A.. University Of New South Wales; Australia
Fil: Rubio, M.. Universidad de Chile; Chile
Materia
HII REGIONS
ISM: MOLECULES
GALAXIES: ISM
MAGELLANIC CLOUDS
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/21844
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/21844
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling A view of Large Magellanic Cloud H ii regions N159, N132, and N166 through the 345-GHz windowParon, Sergio ArielOrtega, Martin EduardoFariña, CeciliaCunningham, M.Jones, P. A.Rubio, M.HII REGIONSISM: MOLECULESGALAXIES: ISMMAGELLANIC CLOUDShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We present results obtained towards the H II regions N159, N166, and N132 from the emission of several molecular lines in the 345 GHz window. Using Atacama Submillimetre Telescope Experiment, we mapped a 2.4 arcmin × 2.4 arcmin region towards the molecular cloud N159-W in the 13CO J = 3–2 line and observed several molecular lines at an infrared (IR) peak very close to a massive young stellar object. 12CO and 13CO J = 3–2 were observed towards two positions in N166 and one position in N132. The 13CO J = 3–2 map of the N159-W cloud shows that the molecular peak is shifted south-west compared to the peak of the IR emission. Towards the IR peak, we detected emission from HCN, HNC, HCO+, C2H J = 4–3, CS J = 7–6, and tentatively C18O J = 3–2. This is the first reported detection of these molecular lines in N159-W. The analysis of the C2H line yields more evidence supporting that the chemistry involving this molecular species in compact and/or UC H II regions in the Large Magellanic Cloud should be similar to that in Galactic ones. A non-LTE (local thermodynamic equilibrium) study of the CO emission suggests the presence of both cool and warm gas in the analysed region. The same analysis for the CS, HCO+, HCN, and HNC shows that it is very likely that their emissions arise mainly from warm gas with a density between 5 × 105 to some 106 cm−3. The obtained HCN/HNC abundance ratio greater than 1 is compatible with warm gas and with an star-forming scenario. From the analysis of the molecular lines observed towards N132 and N166, we propose that both regions should have similar physical conditions, with densities of about 103 cm−3.Fil: Paron, Sergio Ariel. 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; ArgentinaFil: Ortega, Martin Eduardo. 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; ArgentinaFil: Fariña, Cecilia. Grupo de Telescopios Isaac Newton; España. Consejo Nacional de Investigaciones Científicas y Técnicas; ArgentinaFil: Cunningham, M.. University Of New South Wales; AustraliaFil: Jones, P. A.. University Of New South Wales; AustraliaFil: Rubio, M.. Universidad de Chile; ChileOxford University Press2015-11info: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/11336/21844Paron, Sergio Ariel; Ortega, Martin Eduardo; Fariña, Cecilia; Cunningham, M.; Jones, P. A.; et al.; A view of Large Magellanic Cloud H ii regions N159, N132, and N166 through the 345-GHz window; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 455; 1; 11-2015; 518-5250035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stv2326info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/455/1/518/985524/A-view-of-Large-Magellanic-Cloud-H-ii-regions-N159info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1510.01246info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T14:39:48Zoai:ri.conicet.gov.ar:11336/21844instacron: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:34982025-10-15 14:39:48.777CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv A view of Large Magellanic Cloud H ii regions N159, N132, and N166 through the 345-GHz window
title A view of Large Magellanic Cloud H ii regions N159, N132, and N166 through the 345-GHz window
spellingShingle A view of Large Magellanic Cloud H ii regions N159, N132, and N166 through the 345-GHz window
Paron, Sergio Ariel
HII REGIONS
ISM: MOLECULES
GALAXIES: ISM
MAGELLANIC CLOUDS
title_short A view of Large Magellanic Cloud H ii regions N159, N132, and N166 through the 345-GHz window
title_full A view of Large Magellanic Cloud H ii regions N159, N132, and N166 through the 345-GHz window
title_fullStr A view of Large Magellanic Cloud H ii regions N159, N132, and N166 through the 345-GHz window
title_full_unstemmed A view of Large Magellanic Cloud H ii regions N159, N132, and N166 through the 345-GHz window
title_sort A view of Large Magellanic Cloud H ii regions N159, N132, and N166 through the 345-GHz window
dc.creator.none.fl_str_mv Paron, Sergio Ariel
Ortega, Martin Eduardo
Fariña, Cecilia
Cunningham, M.
Jones, P. A.
Rubio, M.
author Paron, Sergio Ariel
author_facet Paron, Sergio Ariel
Ortega, Martin Eduardo
Fariña, Cecilia
Cunningham, M.
Jones, P. A.
Rubio, M.
author_role author
author2 Ortega, Martin Eduardo
Fariña, Cecilia
Cunningham, M.
Jones, P. A.
Rubio, M.
author2_role author
author
author
author
author
dc.subject.none.fl_str_mv HII REGIONS
ISM: MOLECULES
GALAXIES: ISM
MAGELLANIC CLOUDS
topic HII REGIONS
ISM: MOLECULES
GALAXIES: ISM
MAGELLANIC CLOUDS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We present results obtained towards the H II regions N159, N166, and N132 from the emission of several molecular lines in the 345 GHz window. Using Atacama Submillimetre Telescope Experiment, we mapped a 2.4 arcmin × 2.4 arcmin region towards the molecular cloud N159-W in the 13CO J = 3–2 line and observed several molecular lines at an infrared (IR) peak very close to a massive young stellar object. 12CO and 13CO J = 3–2 were observed towards two positions in N166 and one position in N132. The 13CO J = 3–2 map of the N159-W cloud shows that the molecular peak is shifted south-west compared to the peak of the IR emission. Towards the IR peak, we detected emission from HCN, HNC, HCO+, C2H J = 4–3, CS J = 7–6, and tentatively C18O J = 3–2. This is the first reported detection of these molecular lines in N159-W. The analysis of the C2H line yields more evidence supporting that the chemistry involving this molecular species in compact and/or UC H II regions in the Large Magellanic Cloud should be similar to that in Galactic ones. A non-LTE (local thermodynamic equilibrium) study of the CO emission suggests the presence of both cool and warm gas in the analysed region. The same analysis for the CS, HCO+, HCN, and HNC shows that it is very likely that their emissions arise mainly from warm gas with a density between 5 × 105 to some 106 cm−3. The obtained HCN/HNC abundance ratio greater than 1 is compatible with warm gas and with an star-forming scenario. From the analysis of the molecular lines observed towards N132 and N166, we propose that both regions should have similar physical conditions, with densities of about 103 cm−3.
Fil: Paron, Sergio Ariel. 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
Fil: Ortega, Martin Eduardo. 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
Fil: Fariña, Cecilia. Grupo de Telescopios Isaac Newton; España. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina
Fil: Cunningham, M.. University Of New South Wales; Australia
Fil: Jones, P. A.. University Of New South Wales; Australia
Fil: Rubio, M.. Universidad de Chile; Chile
description We present results obtained towards the H II regions N159, N166, and N132 from the emission of several molecular lines in the 345 GHz window. Using Atacama Submillimetre Telescope Experiment, we mapped a 2.4 arcmin × 2.4 arcmin region towards the molecular cloud N159-W in the 13CO J = 3–2 line and observed several molecular lines at an infrared (IR) peak very close to a massive young stellar object. 12CO and 13CO J = 3–2 were observed towards two positions in N166 and one position in N132. The 13CO J = 3–2 map of the N159-W cloud shows that the molecular peak is shifted south-west compared to the peak of the IR emission. Towards the IR peak, we detected emission from HCN, HNC, HCO+, C2H J = 4–3, CS J = 7–6, and tentatively C18O J = 3–2. This is the first reported detection of these molecular lines in N159-W. The analysis of the C2H line yields more evidence supporting that the chemistry involving this molecular species in compact and/or UC H II regions in the Large Magellanic Cloud should be similar to that in Galactic ones. A non-LTE (local thermodynamic equilibrium) study of the CO emission suggests the presence of both cool and warm gas in the analysed region. The same analysis for the CS, HCO+, HCN, and HNC shows that it is very likely that their emissions arise mainly from warm gas with a density between 5 × 105 to some 106 cm−3. The obtained HCN/HNC abundance ratio greater than 1 is compatible with warm gas and with an star-forming scenario. From the analysis of the molecular lines observed towards N132 and N166, we propose that both regions should have similar physical conditions, with densities of about 103 cm−3.
publishDate 2015
dc.date.none.fl_str_mv 2015-11
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/11336/21844
Paron, Sergio Ariel; Ortega, Martin Eduardo; Fariña, Cecilia; Cunningham, M.; Jones, P. A.; et al.; A view of Large Magellanic Cloud H ii regions N159, N132, and N166 through the 345-GHz window; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 455; 1; 11-2015; 518-525
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/21844
identifier_str_mv Paron, Sergio Ariel; Ortega, Martin Eduardo; Fariña, Cecilia; Cunningham, M.; Jones, P. A.; et al.; A view of Large Magellanic Cloud H ii regions N159, N132, and N166 through the 345-GHz window; Oxford University Press; Monthly Notices of the Royal Astronomical Society; 455; 1; 11-2015; 518-525
0035-8711
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/stv2326
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/455/1/518/985524/A-view-of-Large-Magellanic-Cloud-H-ii-regions-N159
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1510.01246
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
application/pdf
application/pdf
application/pdf
dc.publisher.none.fl_str_mv Oxford University Press
publisher.none.fl_str_mv Oxford University Press
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 13.22299

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