Mapping the 13CO/C18O abundance ratio in the massive star-forming region G29.96-0.02

Autores
Paron, Sergio Ariel; Areal, María Belén; Ortega, Martin Eduardo
Año de publicación
2018
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Aims. Estimating molecular abundances ratios from directly measuring the emission of the molecules toward a variety of interstellar environments is indeed very useful to advance our understanding of the chemical evolution of the Galaxy, and hence of the physical processes related to the chemistry. It is necessary to increase the sample of molecular clouds, located at different distances, in which the behavior of molecular abundance ratios, such as the 13CO/C18O ratio, is studied in detail. Methods. We selected the well-studied high-mass star-forming region G29.96-0.02, located at a distance of about 6.2 kpc, which is an ideal laboratory to perform this type of study. To study the 13CO/C18O abundance ratio (X13/18) toward this region, we used 12CO J = 3-2 data obtained from the CO High-Resolution Survey, 13CO and C18O J = 3-2 data from the 13CO/C18O (J = 3-2) Heterodyne Inner Milky Way Plane Survey, and 13CO and C18O J = 2-1 data retrieved from the CDS database that were observed with the IRAM 30 m telescope. The distribution of column densities and X13/18 throughout the extension of the analyzed molecular cloud was studied based on local thermal equilibrium (LTE) and non-LTE methods. Results. Values of X13/18 between 1.5 and 10.5, with an average of about 5, were found throughout the studied region, showing that in addition to the dependency of X13/18 and the galactocentric distance, the local physical conditions may strongly affect this abundance ratio. We found that correlating the X13/18 map with the location of the ionized gas and dark clouds allows us to suggest in which regions the far-UV radiation stalls in dense gaseous components, and in which regions it escapes and selectively photodissociates the C18O isotope. The non-LTE analysis shows that the molecular gas has very different physical conditions, not only spatially throughout the cloud, but also along the line of sight. This type of study may represent a tool for indirectly estimating (from molecular line observations) the degree of photodissociation in molecular clouds, which is indeed useful to study the chemistry in the interstellar medium.
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: Areal, María Belén. 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
Materia
GALAXY: ABUNDANCES
HII REGIONS
ISM: ABUNDANCES
ISM: MOLECULES
STARS: FORMATION
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:11336/86368

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network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Mapping the 13CO/C18O abundance ratio in the massive star-forming region G29.96-0.02Paron, Sergio ArielAreal, María BelénOrtega, Martin EduardoGALAXY: ABUNDANCESHII REGIONSISM: ABUNDANCESISM: MOLECULESSTARS: FORMATIONhttps://purl.org/becyt/ford/1.7https://purl.org/becyt/ford/1Aims. Estimating molecular abundances ratios from directly measuring the emission of the molecules toward a variety of interstellar environments is indeed very useful to advance our understanding of the chemical evolution of the Galaxy, and hence of the physical processes related to the chemistry. It is necessary to increase the sample of molecular clouds, located at different distances, in which the behavior of molecular abundance ratios, such as the 13CO/C18O ratio, is studied in detail. Methods. We selected the well-studied high-mass star-forming region G29.96-0.02, located at a distance of about 6.2 kpc, which is an ideal laboratory to perform this type of study. To study the 13CO/C18O abundance ratio (X13/18) toward this region, we used 12CO J = 3-2 data obtained from the CO High-Resolution Survey, 13CO and C18O J = 3-2 data from the 13CO/C18O (J = 3-2) Heterodyne Inner Milky Way Plane Survey, and 13CO and C18O J = 2-1 data retrieved from the CDS database that were observed with the IRAM 30 m telescope. The distribution of column densities and X13/18 throughout the extension of the analyzed molecular cloud was studied based on local thermal equilibrium (LTE) and non-LTE methods. Results. Values of X13/18 between 1.5 and 10.5, with an average of about 5, were found throughout the studied region, showing that in addition to the dependency of X13/18 and the galactocentric distance, the local physical conditions may strongly affect this abundance ratio. We found that correlating the X13/18 map with the location of the ionized gas and dark clouds allows us to suggest in which regions the far-UV radiation stalls in dense gaseous components, and in which regions it escapes and selectively photodissociates the C18O isotope. The non-LTE analysis shows that the molecular gas has very different physical conditions, not only spatially throughout the cloud, but also along the line of sight. This type of study may represent a tool for indirectly estimating (from molecular line observations) the degree of photodissociation in molecular clouds, which is indeed useful to study the chemistry in the interstellar medium.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: Areal, María Belén. 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; ArgentinaEDP Sciences2018-09info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/86368Paron, Sergio Ariel; Areal, María Belén; Ortega, Martin Eduardo; Mapping the 13CO/C18O abundance ratio in the massive star-forming region G29.96-0.02; EDP Sciences; Astronomy and Astrophysics; 617; A14; 9-2018; 1-80004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/abs/2018A%26A...617A..14Pinfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201833658info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T09:36:19Zoai:ri.conicet.gov.ar:11336/86368instacron: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:34982025-09-29 09:36:20.15CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Mapping the 13CO/C18O abundance ratio in the massive star-forming region G29.96-0.02
title Mapping the 13CO/C18O abundance ratio in the massive star-forming region G29.96-0.02
spellingShingle Mapping the 13CO/C18O abundance ratio in the massive star-forming region G29.96-0.02
Paron, Sergio Ariel
GALAXY: ABUNDANCES
HII REGIONS
ISM: ABUNDANCES
ISM: MOLECULES
STARS: FORMATION
title_short Mapping the 13CO/C18O abundance ratio in the massive star-forming region G29.96-0.02
title_full Mapping the 13CO/C18O abundance ratio in the massive star-forming region G29.96-0.02
title_fullStr Mapping the 13CO/C18O abundance ratio in the massive star-forming region G29.96-0.02
title_full_unstemmed Mapping the 13CO/C18O abundance ratio in the massive star-forming region G29.96-0.02
title_sort Mapping the 13CO/C18O abundance ratio in the massive star-forming region G29.96-0.02
dc.creator.none.fl_str_mv Paron, Sergio Ariel
Areal, María Belén
Ortega, Martin Eduardo
author Paron, Sergio Ariel
author_facet Paron, Sergio Ariel
Areal, María Belén
Ortega, Martin Eduardo
author_role author
author2 Areal, María Belén
Ortega, Martin Eduardo
author2_role author
author
dc.subject.none.fl_str_mv GALAXY: ABUNDANCES
HII REGIONS
ISM: ABUNDANCES
ISM: MOLECULES
STARS: FORMATION
topic GALAXY: ABUNDANCES
HII REGIONS
ISM: ABUNDANCES
ISM: MOLECULES
STARS: FORMATION
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.7
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Aims. Estimating molecular abundances ratios from directly measuring the emission of the molecules toward a variety of interstellar environments is indeed very useful to advance our understanding of the chemical evolution of the Galaxy, and hence of the physical processes related to the chemistry. It is necessary to increase the sample of molecular clouds, located at different distances, in which the behavior of molecular abundance ratios, such as the 13CO/C18O ratio, is studied in detail. Methods. We selected the well-studied high-mass star-forming region G29.96-0.02, located at a distance of about 6.2 kpc, which is an ideal laboratory to perform this type of study. To study the 13CO/C18O abundance ratio (X13/18) toward this region, we used 12CO J = 3-2 data obtained from the CO High-Resolution Survey, 13CO and C18O J = 3-2 data from the 13CO/C18O (J = 3-2) Heterodyne Inner Milky Way Plane Survey, and 13CO and C18O J = 2-1 data retrieved from the CDS database that were observed with the IRAM 30 m telescope. The distribution of column densities and X13/18 throughout the extension of the analyzed molecular cloud was studied based on local thermal equilibrium (LTE) and non-LTE methods. Results. Values of X13/18 between 1.5 and 10.5, with an average of about 5, were found throughout the studied region, showing that in addition to the dependency of X13/18 and the galactocentric distance, the local physical conditions may strongly affect this abundance ratio. We found that correlating the X13/18 map with the location of the ionized gas and dark clouds allows us to suggest in which regions the far-UV radiation stalls in dense gaseous components, and in which regions it escapes and selectively photodissociates the C18O isotope. The non-LTE analysis shows that the molecular gas has very different physical conditions, not only spatially throughout the cloud, but also along the line of sight. This type of study may represent a tool for indirectly estimating (from molecular line observations) the degree of photodissociation in molecular clouds, which is indeed useful to study the chemistry in the interstellar medium.
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: Areal, María Belén. 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
description Aims. Estimating molecular abundances ratios from directly measuring the emission of the molecules toward a variety of interstellar environments is indeed very useful to advance our understanding of the chemical evolution of the Galaxy, and hence of the physical processes related to the chemistry. It is necessary to increase the sample of molecular clouds, located at different distances, in which the behavior of molecular abundance ratios, such as the 13CO/C18O ratio, is studied in detail. Methods. We selected the well-studied high-mass star-forming region G29.96-0.02, located at a distance of about 6.2 kpc, which is an ideal laboratory to perform this type of study. To study the 13CO/C18O abundance ratio (X13/18) toward this region, we used 12CO J = 3-2 data obtained from the CO High-Resolution Survey, 13CO and C18O J = 3-2 data from the 13CO/C18O (J = 3-2) Heterodyne Inner Milky Way Plane Survey, and 13CO and C18O J = 2-1 data retrieved from the CDS database that were observed with the IRAM 30 m telescope. The distribution of column densities and X13/18 throughout the extension of the analyzed molecular cloud was studied based on local thermal equilibrium (LTE) and non-LTE methods. Results. Values of X13/18 between 1.5 and 10.5, with an average of about 5, were found throughout the studied region, showing that in addition to the dependency of X13/18 and the galactocentric distance, the local physical conditions may strongly affect this abundance ratio. We found that correlating the X13/18 map with the location of the ionized gas and dark clouds allows us to suggest in which regions the far-UV radiation stalls in dense gaseous components, and in which regions it escapes and selectively photodissociates the C18O isotope. The non-LTE analysis shows that the molecular gas has very different physical conditions, not only spatially throughout the cloud, but also along the line of sight. This type of study may represent a tool for indirectly estimating (from molecular line observations) the degree of photodissociation in molecular clouds, which is indeed useful to study the chemistry in the interstellar medium.
publishDate 2018
dc.date.none.fl_str_mv 2018-09
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/11336/86368
Paron, Sergio Ariel; Areal, María Belén; Ortega, Martin Eduardo; Mapping the 13CO/C18O abundance ratio in the massive star-forming region G29.96-0.02; EDP Sciences; Astronomy and Astrophysics; 617; A14; 9-2018; 1-8
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/86368
identifier_str_mv Paron, Sergio Ariel; Areal, María Belén; Ortega, Martin Eduardo; Mapping the 13CO/C18O abundance ratio in the massive star-forming region G29.96-0.02; EDP Sciences; Astronomy and Astrophysics; 617; A14; 9-2018; 1-8
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/http://adsabs.harvard.edu/abs/2018A%26A...617A..14P
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201833658
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
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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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