Formation and evolution of globular clusters in the Galaxy and Magellanic Clouds

Detalhes bibliográficos
Autor(a) principal: Dias, Bruno Moreira de Souza
Data de Publicação: 2014
Tipo de documento: Tese
Idioma: eng
Título da fonte: Biblioteca Digital de Teses e Dissertações da USP
Texto Completo: http://www.teses.usp.br/teses/disponiveis/14/14131/tde-26082014-090039/
Resumo: Globular clusters are tracers of the formation and evolution of their host galaxies. Kinematics, chemical abundances, age and position of the clusters allows tracing interactions between Milky Way and surrounding galaxies and outlines their chemical enrichment history. In this thesis we analyse mid-resolution spectra of about 800 red giant stars in 51 Galactic globular clusters. It is the first time that [Fe/H] and [Mg/Fe] derived in a consistent way are published for such a huge sample of globular clusters, almost 1/3 of the total number of catalogued clusters. Our metallicities are showed to be more precise than previous works based on mid-resolution spectroscopy. A turnover at [Fe/H] ~ -1.0 is found in the plot [Fe/H] vs. [Mg/Fe] for bulge and halo, although bulge seems to have a more metal-rich turnover, i.e, bulge has more efficient formation than the halo. Comparing the abundances with age the timescale for SNIa to start to become important is 1Gyr. [Fe/H] vs. age corroborates the different star formation efficiency of bulge and halo while [Mg/Fe] does not follow that. Halo was formed in mini halos or dwarf galaxies, and two multiple population clusters had their origin analysed to check it. M 22 seems to have been formed in the Milky Way while NGC 5824 possibly was originated in a dwarf galaxy, although our results are inconclusive for NGC 5824. The Galactic bulge seems to have been formed fast i.e., probably the oldest globular cluster is there. In fact HP 1 has a bluer horizontal branch than expected for its metallicity and we interpret that as an age effect. We determine its distance using light curves of variable stars in order to constrain future age determinations via colour-magnitude diagram. Finally, we investigate interaction between Milky Way and its neighbour galaxy SMC. We find that some star clusters are being stripped out of the SMC main body, which is consistent with tidal stripping scenario for the interaction between the galaxies, instead of ram pressure that would only affect gas.
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spelling Formation and evolution of globular clusters in the Galaxy and Magellanic CloudsFormação e evolução de aglomerados globulares da Galáxia e Nuvens de Magalhãesdiagramas Hertzprung-Russell e cor-magnitudeEstrelas: abundâncias Estrelas: cinemática e dinâmicaEstrelas: População IIEstrelas: variáveis: RR LyraeGaláxia: aglomerados globularesGaláxia: bojoGaláxia: conteúdo estelarGaláxia: evoluçãoGaláxia: formaçãoGaláxia: haloGaláxias: aglomerados de estrelas: geralGalaxies: star clusters: generalGalaxy: bulgeGalaxy: evolutionGalaxy: formationGalaxy: globular clustersGalaxy: haloGalaxy: stellar contentsHertzprung-Russell and colour-magnitude diagramsMagellanic CloudsNuvens de MagalhãesStars: abundancesStars: kinematics and dynamicsStars: Population IIStars: variables: RR LyraeGlobular clusters are tracers of the formation and evolution of their host galaxies. Kinematics, chemical abundances, age and position of the clusters allows tracing interactions between Milky Way and surrounding galaxies and outlines their chemical enrichment history. In this thesis we analyse mid-resolution spectra of about 800 red giant stars in 51 Galactic globular clusters. It is the first time that [Fe/H] and [Mg/Fe] derived in a consistent way are published for such a huge sample of globular clusters, almost 1/3 of the total number of catalogued clusters. Our metallicities are showed to be more precise than previous works based on mid-resolution spectroscopy. A turnover at [Fe/H] ~ -1.0 is found in the plot [Fe/H] vs. [Mg/Fe] for bulge and halo, although bulge seems to have a more metal-rich turnover, i.e, bulge has more efficient formation than the halo. Comparing the abundances with age the timescale for SNIa to start to become important is 1Gyr. [Fe/H] vs. age corroborates the different star formation efficiency of bulge and halo while [Mg/Fe] does not follow that. Halo was formed in mini halos or dwarf galaxies, and two multiple population clusters had their origin analysed to check it. M 22 seems to have been formed in the Milky Way while NGC 5824 possibly was originated in a dwarf galaxy, although our results are inconclusive for NGC 5824. The Galactic bulge seems to have been formed fast i.e., probably the oldest globular cluster is there. In fact HP 1 has a bluer horizontal branch than expected for its metallicity and we interpret that as an age effect. We determine its distance using light curves of variable stars in order to constrain future age determinations via colour-magnitude diagram. Finally, we investigate interaction between Milky Way and its neighbour galaxy SMC. We find that some star clusters are being stripped out of the SMC main body, which is consistent with tidal stripping scenario for the interaction between the galaxies, instead of ram pressure that would only affect gas.Aglomerados globulares são traçadores da formação e evolução de suas galáxias. Cinemática, abundâncias químicas, idades e posições dos aglomerados permitem traçar interações entre Via Láctea e galáxias vizinhas e suas histórias de enriquecimento químico. Nesta tese analisamos espectros de média resolução de mais de 800 estrelas gigantes vermelhas em 51 aglomerados globulares Galácticos. É a primeira vez que [Fe/H] and [Mg/Fe] determinados de modo consistente são publicados para uma amostra desse porte, ~1/3 dos objetos catalogados. Nossas metalicidades são mais precisas que trabalhos anteriores similares. Uma quebra em [Fe/H] ~ -1.0 é encontrada no gráfico [Fe/H] vs. [Mg/Fe] para o bojo e halo, embora bojo parece ter uma quebra em [Fe/H] maior, i.e, bojo tem formaçãao mais eficiente que o halo. Comparando abundâncias com idade, a escala de tempo para SNIa ficar importante é 1Gano. [Fe/H] vs. idade corrobora diferentes eficiências de formação do bojo e halo, mas [Mg/Fe] vs. idade não mostra isso. O halo foi formado em mini halos ou galáxias anãs, e dois aglomerados com dispersão em [Fe/H] tiveram suas origens analisadas. M 22 parece ter sido formado na Via Láctea e NGC 5824 possivelmente foi originado em uma galáxia anã, embora os resultados são inconclusivos para NGC 5824. O bojo parece ter sido formado rapidamente e deve possuir o aglomerado mais velho. De fato, HP 1 tem um ramo horizontal mais azul que o esperado para sua metalicidade e vemos isso como um efeito da idade. Determinamos sua distância usando curvas de luz de RR Lyrae de maneira a restringir futuras determinações de idade via diagrama cor-magnitude. Finalmente, investigamos a interação entre Via Láctea e sua galáxia vizinha SMC. Encontramos aglomerados sendo removidos do corpo central da SMC, consistente com cenário de remoção por força de maré para a interação entre as galáxias, em vez de ``ram pressure\'\' que afeta só gás.Biblioteca Digitais de Teses e Dissertações da USPBarbuy, Beatriz Leonor SilveiraDias, Bruno Moreira de Souza2014-06-25info:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/doctoralThesisapplication/pdfhttp://www.teses.usp.br/teses/disponiveis/14/14131/tde-26082014-090039/reponame:Biblioteca Digital de Teses e Dissertações da USPinstname:Universidade de São Paulo (USP)instacron:USPLiberar o conteúdo para acesso público.info:eu-repo/semantics/openAccesseng2016-07-28T16:11:55Zoai:teses.usp.br:tde-26082014-090039Biblioteca Digital de Teses e Dissertaçõeshttp://www.teses.usp.br/PUBhttp://www.teses.usp.br/cgi-bin/mtd2br.plvirginia@if.usp.br|| atendimento@aguia.usp.br||virginia@if.usp.bropendoar:27212016-07-28T16:11:55Biblioteca Digital de Teses e Dissertações da USP - Universidade de São Paulo (USP)false
dc.title.none.fl_str_mv Formation and evolution of globular clusters in the Galaxy and Magellanic Clouds
Formação e evolução de aglomerados globulares da Galáxia e Nuvens de Magalhães
title Formation and evolution of globular clusters in the Galaxy and Magellanic Clouds
spellingShingle Formation and evolution of globular clusters in the Galaxy and Magellanic Clouds
Dias, Bruno Moreira de Souza
diagramas Hertzprung-Russell e cor-magnitude
Estrelas: abundâncias Estrelas: cinemática e dinâmica
Estrelas: População II
Estrelas: variáveis: RR Lyrae
Galáxia: aglomerados globulares
Galáxia: bojo
Galáxia: conteúdo estelar
Galáxia: evolução
Galáxia: formação
Galáxia: halo
Galáxias: aglomerados de estrelas: geral
Galaxies: star clusters: general
Galaxy: bulge
Galaxy: evolution
Galaxy: formation
Galaxy: globular clusters
Galaxy: halo
Galaxy: stellar contents
Hertzprung-Russell and colour-magnitude diagrams
Magellanic Clouds
Nuvens de Magalhães
Stars: abundances
Stars: kinematics and dynamics
Stars: Population II
Stars: variables: RR Lyrae
title_short Formation and evolution of globular clusters in the Galaxy and Magellanic Clouds
title_full Formation and evolution of globular clusters in the Galaxy and Magellanic Clouds
title_fullStr Formation and evolution of globular clusters in the Galaxy and Magellanic Clouds
title_full_unstemmed Formation and evolution of globular clusters in the Galaxy and Magellanic Clouds
title_sort Formation and evolution of globular clusters in the Galaxy and Magellanic Clouds
author Dias, Bruno Moreira de Souza
author_facet Dias, Bruno Moreira de Souza
author_role author
dc.contributor.none.fl_str_mv Barbuy, Beatriz Leonor Silveira
dc.contributor.author.fl_str_mv Dias, Bruno Moreira de Souza
dc.subject.por.fl_str_mv diagramas Hertzprung-Russell e cor-magnitude
Estrelas: abundâncias Estrelas: cinemática e dinâmica
Estrelas: População II
Estrelas: variáveis: RR Lyrae
Galáxia: aglomerados globulares
Galáxia: bojo
Galáxia: conteúdo estelar
Galáxia: evolução
Galáxia: formação
Galáxia: halo
Galáxias: aglomerados de estrelas: geral
Galaxies: star clusters: general
Galaxy: bulge
Galaxy: evolution
Galaxy: formation
Galaxy: globular clusters
Galaxy: halo
Galaxy: stellar contents
Hertzprung-Russell and colour-magnitude diagrams
Magellanic Clouds
Nuvens de Magalhães
Stars: abundances
Stars: kinematics and dynamics
Stars: Population II
Stars: variables: RR Lyrae
topic diagramas Hertzprung-Russell e cor-magnitude
Estrelas: abundâncias Estrelas: cinemática e dinâmica
Estrelas: População II
Estrelas: variáveis: RR Lyrae
Galáxia: aglomerados globulares
Galáxia: bojo
Galáxia: conteúdo estelar
Galáxia: evolução
Galáxia: formação
Galáxia: halo
Galáxias: aglomerados de estrelas: geral
Galaxies: star clusters: general
Galaxy: bulge
Galaxy: evolution
Galaxy: formation
Galaxy: globular clusters
Galaxy: halo
Galaxy: stellar contents
Hertzprung-Russell and colour-magnitude diagrams
Magellanic Clouds
Nuvens de Magalhães
Stars: abundances
Stars: kinematics and dynamics
Stars: Population II
Stars: variables: RR Lyrae
description Globular clusters are tracers of the formation and evolution of their host galaxies. Kinematics, chemical abundances, age and position of the clusters allows tracing interactions between Milky Way and surrounding galaxies and outlines their chemical enrichment history. In this thesis we analyse mid-resolution spectra of about 800 red giant stars in 51 Galactic globular clusters. It is the first time that [Fe/H] and [Mg/Fe] derived in a consistent way are published for such a huge sample of globular clusters, almost 1/3 of the total number of catalogued clusters. Our metallicities are showed to be more precise than previous works based on mid-resolution spectroscopy. A turnover at [Fe/H] ~ -1.0 is found in the plot [Fe/H] vs. [Mg/Fe] for bulge and halo, although bulge seems to have a more metal-rich turnover, i.e, bulge has more efficient formation than the halo. Comparing the abundances with age the timescale for SNIa to start to become important is 1Gyr. [Fe/H] vs. age corroborates the different star formation efficiency of bulge and halo while [Mg/Fe] does not follow that. Halo was formed in mini halos or dwarf galaxies, and two multiple population clusters had their origin analysed to check it. M 22 seems to have been formed in the Milky Way while NGC 5824 possibly was originated in a dwarf galaxy, although our results are inconclusive for NGC 5824. The Galactic bulge seems to have been formed fast i.e., probably the oldest globular cluster is there. In fact HP 1 has a bluer horizontal branch than expected for its metallicity and we interpret that as an age effect. We determine its distance using light curves of variable stars in order to constrain future age determinations via colour-magnitude diagram. Finally, we investigate interaction between Milky Way and its neighbour galaxy SMC. We find that some star clusters are being stripped out of the SMC main body, which is consistent with tidal stripping scenario for the interaction between the galaxies, instead of ram pressure that would only affect gas.
publishDate 2014
dc.date.none.fl_str_mv 2014-06-25
dc.type.status.fl_str_mv info:eu-repo/semantics/publishedVersion
dc.type.driver.fl_str_mv info:eu-repo/semantics/doctoralThesis
format doctoralThesis
status_str publishedVersion
dc.identifier.uri.fl_str_mv http://www.teses.usp.br/teses/disponiveis/14/14131/tde-26082014-090039/
url http://www.teses.usp.br/teses/disponiveis/14/14131/tde-26082014-090039/
dc.language.iso.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv
dc.rights.driver.fl_str_mv Liberar o conteúdo para acesso público.
info:eu-repo/semantics/openAccess
rights_invalid_str_mv Liberar o conteúdo para acesso público.
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.coverage.none.fl_str_mv
dc.publisher.none.fl_str_mv Biblioteca Digitais de Teses e Dissertações da USP
publisher.none.fl_str_mv Biblioteca Digitais de Teses e Dissertações da USP
dc.source.none.fl_str_mv
reponame:Biblioteca Digital de Teses e Dissertações da USP
instname:Universidade de São Paulo (USP)
instacron:USP
instname_str Universidade de São Paulo (USP)
instacron_str USP
institution USP
reponame_str Biblioteca Digital de Teses e Dissertações da USP
collection Biblioteca Digital de Teses e Dissertações da USP
repository.name.fl_str_mv Biblioteca Digital de Teses e Dissertações da USP - Universidade de São Paulo (USP)
repository.mail.fl_str_mv virginia@if.usp.br|| atendimento@aguia.usp.br||virginia@if.usp.br
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