THE PHYSICAL AND KINEMATICAL STRUCTURE OF MASSIVE AND DENSE COLD CORES

In spite of the efforts focused on understanding the formation of high mass stars, we do not have a clear understanding of which are the processes involved. To understand it, we need to characterize objects in very early stages of evolution and therefore infer the initial conditions of these process...

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Detalles Bibliográficos
Autor: Servajean-Bergoeing, Elise Marie Germaine
Tipo de recurso: tesis doctoral
Estado:Versión publicada
Fecha de publicación:2019
País:Chile
OAI Identifier:oai:repositorio.anid.cl:10533/235755
Acceso en línea:https://hdl.handle.net/10533/235755
Access Level:acceso abierto
Palabra clave:Ciencias Naturales
Ciencias Físicas
Astronomía
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dc.title.es_CL.fl_str_mv THE PHYSICAL AND KINEMATICAL STRUCTURE OF MASSIVE AND DENSE COLD CORES
title THE PHYSICAL AND KINEMATICAL STRUCTURE OF MASSIVE AND DENSE COLD CORES
spellingShingle THE PHYSICAL AND KINEMATICAL STRUCTURE OF MASSIVE AND DENSE COLD CORES
Servajean-Bergoeing, Elise Marie Germaine
Ciencias Naturales
Ciencias Físicas
Astronomía
title_short THE PHYSICAL AND KINEMATICAL STRUCTURE OF MASSIVE AND DENSE COLD CORES
title_full THE PHYSICAL AND KINEMATICAL STRUCTURE OF MASSIVE AND DENSE COLD CORES
title_fullStr THE PHYSICAL AND KINEMATICAL STRUCTURE OF MASSIVE AND DENSE COLD CORES
title_full_unstemmed THE PHYSICAL AND KINEMATICAL STRUCTURE OF MASSIVE AND DENSE COLD CORES
title_sort THE PHYSICAL AND KINEMATICAL STRUCTURE OF MASSIVE AND DENSE COLD CORES
dc.creator.none.fl_str_mv Servajean-Bergoeing, Elise Marie Germaine
author Servajean-Bergoeing, Elise Marie Germaine
author_facet Servajean-Bergoeing, Elise Marie Germaine
author_role author
dc.contributor.advisor.none.fl_str_mv Garay-Brignardello, Guido
dc.contributor.institution.es_CL.fl_str_mv UNIVERSIDAD DE CHILE
dc.subject.oecd1n.es_CL.fl_str_mv Ciencias Naturales
topic Ciencias Naturales
Ciencias Físicas
Astronomía
dc.subject.oecd2n.es_CL.fl_str_mv Ciencias Físicas
dc.subject.oecd3n.es_CL.fl_str_mv Astronomía
description In spite of the efforts focused on understanding the formation of high mass stars, we do not have a clear understanding of which are the processes involved. To understand it, we need to characterize objects in very early stages of evolution and therefore infer the initial conditions of these processes. In this thesis, we study these objects from two different perspectives. First, we characterized four cold, dense, and massive clumps in the early stages of evolution (G305.136+0.068, G333.125- 0.562, G18.606-0.076, and G34.458+0.121), and we analyzed which are their collapse signatures. This was done using data from the Atacama Pathfinder Experiment (APEX) with an angular resolution of ∼20”. On the other hand, we studied the mass distribution within the quieter object (G305.136+0.068) using data from the Atacama Large Millimeter/submillimeter Array (ALMA) with high angular resolution (∼2”), being able to detect the small fragments that will become star seeds. The four objects observed with APEX show various kinematical characteristics showing different stages of evolution. In all the objects the molecular line velocity dispersions are broader than the thermal widths implying other types of processes like turbulence and/or collapse. The viral analysis of the objects indicates that they are likely to be bound. For two of the studied objects (G305.136+0.068, and G333.125-0.562), we found clear collapse signatures in the molecular line profiles. Regarding the ALMA observations towards G305.136+0.069, the dust continuum observations reveal the presence of twelve compact structures (cores) with masses ranging from 3.3 to 50.6 M⊙ and radius from 1800 to 5300 AU. The line observations indicate that the fragments are dominated by non-thermal motions. The virial parameters of the three most massive cores suggest that they are undergoing collapse. We find that in the regime of masses probed by our observations (M > 3 M⊙) the shape of the core mass function shows an overpopulation of high mass cores.
publishDate 2019
dc.date.accessioned.none.fl_str_mv 2019-05-31T14:55:48Z
2022-08-16T20:03:37Z
dc.date.available.none.fl_str_mv 2019-05-31T14:55:48Z
2022-08-16T20:03:37Z
dc.date.issued.es_CL.fl_str_mv 2019
dc.type.none.fl_str_mv Tesis Doctorado
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dc.identifier.uri.none.fl_str_mv https://hdl.handle.net/10533/235755
identifier_str_mv 21110496
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spelling UNIVERSIDAD DE CHILEServajean-Bergoeing, Elise Marie Germaine2019https://hdl.handle.net/10533/235755http://purl.org/coar/access_right/c_abf2AstronomíaCiencias FísicasCiencias NaturalesTHE PHYSICAL AND KINEMATICAL STRUCTURE OF MASSIVE AND DENSE COLD CORESGaray-Brignardello, GuidoUNIVERSIDAD DE CHILEChileServajean-Bergoeing, Elise Marie Germaine2019-05-31T14:55:48Z2022-08-16T20:03:37Z2019-05-31T14:55:48Z2022-08-16T20:03:37Z2019In spite of the efforts focused on understanding the formation of high mass stars, we do not have a clear understanding of which are the processes involved. To understand it, we need to characterize objects in very early stages of evolution and therefore infer the initial conditions of these processes. In this thesis, we study these objects from two different perspectives. First, we characterized four cold, dense, and massive clumps in the early stages of evolution (G305.136+0.068, G333.125- 0.562, G18.606-0.076, and G34.458+0.121), and we analyzed which are their collapse signatures. This was done using data from the Atacama Pathfinder Experiment (APEX) with an angular resolution of ∼20”. On the other hand, we studied the mass distribution within the quieter object (G305.136+0.068) using data from the Atacama Large Millimeter/submillimeter Array (ALMA) with high angular resolution (∼2”), being able to detect the small fragments that will become star seeds. The four objects observed with APEX show various kinematical characteristics showing different stages of evolution. In all the objects the molecular line velocity dispersions are broader than the thermal widths implying other types of processes like turbulence and/or collapse. The viral analysis of the objects indicates that they are likely to be bound. For two of the studied objects (G305.136+0.068, and G333.125-0.562), we found clear collapse signatures in the molecular line profiles. Regarding the ALMA observations towards G305.136+0.069, the dust continuum observations reveal the presence of twelve compact structures (cores) with masses ranging from 3.3 to 50.6 M⊙ and radius from 1800 to 5300 AU. The line observations indicate that the fragments are dominated by non-thermal motions. The virial parameters of the three most massive cores suggest that they are undergoing collapse. 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