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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/86368
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oai:ri.conicet.gov.ar:11336/86368 |
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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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13.070432 |