Formation and evolution of globular clusters in the Galaxy and Magellanic Clouds
Autor(a) principal: | |
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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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Biblioteca Digital de Teses e Dissertações da USP |
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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 |
_version_ |
1815257398924804096 |