Early Phases of Star Formation: Testing Chemical Tools
- Autores
- Martinez, Naila Constanza; Paron, Sergio Ariel
- Año de publicación
- 2024
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- The star forming processes strongly influence the ISM chemistry. Nowadays, there are available many high-quality databases at millimeter wavelengths. Using them, it is possible to carry out studies that review and deepen previous results. If these studies involve large samples of sources, it is preferred to use direct tools to study the molecular gas. With the aim of testing these tools such as the use of the HCN/HNC ratio as a thermometer, and the use of H13CO+, HC3N, N2H +, and C2H as “chemical clocks”, we present a molecular line study towards 55 sources representing massive young stellar objects (MYSOs) at different evolutive stages: infrared dark clouds (IRDCs), high-mass protostellar objects (HMPOs), hot molecular cores (HMCs) and ultracompact HII regions (UCHII). We found that the use of HCN/HNC ratio as an universal thermometer in the ISM should be taken with care because the HCN optical depth is a big issue that can affect the method. Hence, this tool should be used only after a careful analysis of the HCN spectrum, checking that no line, neither the main nor the hyperfine ones, present absorption features. We point out that the analysis of the emission of H13CO+, HC3N, N2H +, and C2H could be useful to trace and distinguish regions among IRDCs, HMPOs and HMCs. The molecular line widths of these four species increase from the IRDC to the HMC stage, which can be a consequence of the gas dynamics related to the star-forming processes taking place in the molecular clumps. Our results do not only contribute with more statistics regarding to probe such chemical tools, useful to obtain information in large samples of sources, but also complement previous works through the analysis on other types of sources.
Fil: Martinez, Naila Constanza. 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. Universidad de Buenos Aires; Argentina
Fil: Paron, Sergio Ariel. Universidad de Buenos Aires; Argentina. 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
-
ISM: CLOUDS
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:11336/263185
Ver los metadatos del registro completo
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Early Phases of Star Formation: Testing Chemical ToolsMartinez, Naila ConstanzaParon, Sergio ArielISM: CLOUDSISM: MOLECULESSTARS: FORMATIONhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The star forming processes strongly influence the ISM chemistry. Nowadays, there are available many high-quality databases at millimeter wavelengths. Using them, it is possible to carry out studies that review and deepen previous results. If these studies involve large samples of sources, it is preferred to use direct tools to study the molecular gas. With the aim of testing these tools such as the use of the HCN/HNC ratio as a thermometer, and the use of H13CO+, HC3N, N2H +, and C2H as “chemical clocks”, we present a molecular line study towards 55 sources representing massive young stellar objects (MYSOs) at different evolutive stages: infrared dark clouds (IRDCs), high-mass protostellar objects (HMPOs), hot molecular cores (HMCs) and ultracompact HII regions (UCHII). We found that the use of HCN/HNC ratio as an universal thermometer in the ISM should be taken with care because the HCN optical depth is a big issue that can affect the method. Hence, this tool should be used only after a careful analysis of the HCN spectrum, checking that no line, neither the main nor the hyperfine ones, present absorption features. We point out that the analysis of the emission of H13CO+, HC3N, N2H +, and C2H could be useful to trace and distinguish regions among IRDCs, HMPOs and HMCs. The molecular line widths of these four species increase from the IRDC to the HMC stage, which can be a consequence of the gas dynamics related to the star-forming processes taking place in the molecular clumps. Our results do not only contribute with more statistics regarding to probe such chemical tools, useful to obtain information in large samples of sources, but also complement previous works through the analysis on other types of sources.Fil: Martinez, Naila Constanza. 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. Universidad de Buenos Aires; ArgentinaFil: Paron, Sergio Ariel. Universidad de Buenos Aires; Argentina. 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; ArgentinaNational Astronomical Observatories2024-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/263185Martinez, Naila Constanza; Paron, Sergio Ariel; Early Phases of Star Formation: Testing Chemical Tools; National Astronomical Observatories; Research In Astronomy And Astrophysics; 24; 1; 1-2024; 1-281674-4527CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1088/1674-4527/ad0429info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/2310.09226info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.1088/1674-4527/ad0429info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:16:11Zoai:ri.conicet.gov.ar:11336/263185instacron: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 10:16:12.049CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Early Phases of Star Formation: Testing Chemical Tools |
title |
Early Phases of Star Formation: Testing Chemical Tools |
spellingShingle |
Early Phases of Star Formation: Testing Chemical Tools Martinez, Naila Constanza ISM: CLOUDS ISM: MOLECULES STARS: FORMATION |
title_short |
Early Phases of Star Formation: Testing Chemical Tools |
title_full |
Early Phases of Star Formation: Testing Chemical Tools |
title_fullStr |
Early Phases of Star Formation: Testing Chemical Tools |
title_full_unstemmed |
Early Phases of Star Formation: Testing Chemical Tools |
title_sort |
Early Phases of Star Formation: Testing Chemical Tools |
dc.creator.none.fl_str_mv |
Martinez, Naila Constanza Paron, Sergio Ariel |
author |
Martinez, Naila Constanza |
author_facet |
Martinez, Naila Constanza Paron, Sergio Ariel |
author_role |
author |
author2 |
Paron, Sergio Ariel |
author2_role |
author |
dc.subject.none.fl_str_mv |
ISM: CLOUDS ISM: MOLECULES STARS: FORMATION |
topic |
ISM: CLOUDS ISM: MOLECULES STARS: FORMATION |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
The star forming processes strongly influence the ISM chemistry. Nowadays, there are available many high-quality databases at millimeter wavelengths. Using them, it is possible to carry out studies that review and deepen previous results. If these studies involve large samples of sources, it is preferred to use direct tools to study the molecular gas. With the aim of testing these tools such as the use of the HCN/HNC ratio as a thermometer, and the use of H13CO+, HC3N, N2H +, and C2H as “chemical clocks”, we present a molecular line study towards 55 sources representing massive young stellar objects (MYSOs) at different evolutive stages: infrared dark clouds (IRDCs), high-mass protostellar objects (HMPOs), hot molecular cores (HMCs) and ultracompact HII regions (UCHII). We found that the use of HCN/HNC ratio as an universal thermometer in the ISM should be taken with care because the HCN optical depth is a big issue that can affect the method. Hence, this tool should be used only after a careful analysis of the HCN spectrum, checking that no line, neither the main nor the hyperfine ones, present absorption features. We point out that the analysis of the emission of H13CO+, HC3N, N2H +, and C2H could be useful to trace and distinguish regions among IRDCs, HMPOs and HMCs. The molecular line widths of these four species increase from the IRDC to the HMC stage, which can be a consequence of the gas dynamics related to the star-forming processes taking place in the molecular clumps. Our results do not only contribute with more statistics regarding to probe such chemical tools, useful to obtain information in large samples of sources, but also complement previous works through the analysis on other types of sources. Fil: Martinez, Naila Constanza. 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. Universidad de Buenos Aires; Argentina Fil: Paron, Sergio Ariel. Universidad de Buenos Aires; Argentina. 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 |
The star forming processes strongly influence the ISM chemistry. Nowadays, there are available many high-quality databases at millimeter wavelengths. Using them, it is possible to carry out studies that review and deepen previous results. If these studies involve large samples of sources, it is preferred to use direct tools to study the molecular gas. With the aim of testing these tools such as the use of the HCN/HNC ratio as a thermometer, and the use of H13CO+, HC3N, N2H +, and C2H as “chemical clocks”, we present a molecular line study towards 55 sources representing massive young stellar objects (MYSOs) at different evolutive stages: infrared dark clouds (IRDCs), high-mass protostellar objects (HMPOs), hot molecular cores (HMCs) and ultracompact HII regions (UCHII). We found that the use of HCN/HNC ratio as an universal thermometer in the ISM should be taken with care because the HCN optical depth is a big issue that can affect the method. Hence, this tool should be used only after a careful analysis of the HCN spectrum, checking that no line, neither the main nor the hyperfine ones, present absorption features. We point out that the analysis of the emission of H13CO+, HC3N, N2H +, and C2H could be useful to trace and distinguish regions among IRDCs, HMPOs and HMCs. The molecular line widths of these four species increase from the IRDC to the HMC stage, which can be a consequence of the gas dynamics related to the star-forming processes taking place in the molecular clumps. Our results do not only contribute with more statistics regarding to probe such chemical tools, useful to obtain information in large samples of sources, but also complement previous works through the analysis on other types of sources. |
publishDate |
2024 |
dc.date.none.fl_str_mv |
2024-01 |
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/11336/263185 Martinez, Naila Constanza; Paron, Sergio Ariel; Early Phases of Star Formation: Testing Chemical Tools; National Astronomical Observatories; Research In Astronomy And Astrophysics; 24; 1; 1-2024; 1-28 1674-4527 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/263185 |
identifier_str_mv |
Martinez, Naila Constanza; Paron, Sergio Ariel; Early Phases of Star Formation: Testing Chemical Tools; National Astronomical Observatories; Research In Astronomy And Astrophysics; 24; 1; 1-2024; 1-28 1674-4527 CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.1088/1674-4527/ad0429 info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/2310.09226 info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/article/10.1088/1674-4527/ad0429 |
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 |
dc.publisher.none.fl_str_mv |
National Astronomical Observatories |
publisher.none.fl_str_mv |
National Astronomical Observatories |
dc.source.none.fl_str_mv |
reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
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CONICET Digital (CONICET) |
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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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1844614104769101824 |
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13.070432 |