Gradientes de abundâncias químicas em galáxias espirais
Ano de defesa: | 2006 |
---|---|
Autor(a) principal: | |
Orientador(a): | |
Banca de defesa: | , , , |
Tipo de documento: | Tese |
Tipo de acesso: | Acesso aberto |
Idioma: | por |
Instituição de defesa: |
Universidade Federal de Santa Maria
|
Programa de Pós-Graduação: |
Programa de Pós-Graduação em Física
|
Departamento: |
Física
|
País: |
BR
|
Palavras-chave em Português: | |
Palavras-chave em Inglês: | |
Área do conhecimento CNPq: | |
Link de acesso: | http://repositorio.ufsm.br/handle/1/3939 |
Resumo: | We used photoionization models in order to derive O/H, N/O, and S/O abundance gradients in three isolated barred spiral galaxies (NGC 1365, NGC 925, NGC 1073) and in nine spiral galaxies (NGC 4501, NGC 4571, NGC 4689, NGC 4254, NGC4321, NGC4654, NGC4303, NGC4651, NGC4713) in the Virgo cluster. Our O/H predictions were found to be consistent with some empirical abundance de¬terminations, but are overestimated by a factor of 0.1-0.4 dex when compared to the direct abundance measures. For NGC 1365, our models indicate no abundance break, result suggested in previous works. ln NGC 925, despite the flattening in the R23 = ([O Il].\3727+[0 IlI].\4949+.\5007)/H,B oxygen indicator at galactocentric distances R > 6.0 kpc, our model results did not show any presence of an oxygen abundance break. NGC 1073 seems to be overabundant in nitrogen compared to other spiral galaxies. No gradient of S/O was found in the studied galaxies, and we derived a positive gradient for the ionizing star temperatures of the nebulae Teff of L:.Teff /6R = (400 ::I:: 112) K kpc -1 and the logarithmic of the ionizing parameter log U ranging from -3.0 to -2.3. The N/O vs. O/H diagram derived from our results for isolated galaxies is in general consistent with chemical evolution models that assume that the nitrogen synthesis has both a primary and a secondary com¬ponent compared to oxygen. However, a very strong N/O dependence on the O/H at high abundances was found. Our models indicate that galaxies near to the core ofthe Virgo cluster are overabundant in O/H, N/O, and S/O by about 0.25 dex in comparison to the ones at the periphery. With one exception, models with upper stellar mass limit of Mu= 30-40 M0 and age of the ionizing star cluster ranging from 1.5 to 2.5 Myr were able to reproduce the observational data. Chemical evolution models indicate that the collapse time-scale for the inner regions of the galaxies near to the Virgo core is larger than the one in galaxies located at the intermediate and peripheral positions in the cluster, what can be due to the dense environment existing in the Virgo cluster core. |
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2017-05-092017-05-092006-06-28DORS JUNIOR, Oli Luiz. Chemical gradients of abundâncias in galaxies spirals. 2006. 111 f. Tese (Doutorado em Física) - Universidade Federal de Santa Maria, Santa Maria, 2006.http://repositorio.ufsm.br/handle/1/3939We used photoionization models in order to derive O/H, N/O, and S/O abundance gradients in three isolated barred spiral galaxies (NGC 1365, NGC 925, NGC 1073) and in nine spiral galaxies (NGC 4501, NGC 4571, NGC 4689, NGC 4254, NGC4321, NGC4654, NGC4303, NGC4651, NGC4713) in the Virgo cluster. Our O/H predictions were found to be consistent with some empirical abundance de¬terminations, but are overestimated by a factor of 0.1-0.4 dex when compared to the direct abundance measures. For NGC 1365, our models indicate no abundance break, result suggested in previous works. ln NGC 925, despite the flattening in the R23 = ([O Il].\3727+[0 IlI].\4949+.\5007)/H,B oxygen indicator at galactocentric distances R > 6.0 kpc, our model results did not show any presence of an oxygen abundance break. NGC 1073 seems to be overabundant in nitrogen compared to other spiral galaxies. No gradient of S/O was found in the studied galaxies, and we derived a positive gradient for the ionizing star temperatures of the nebulae Teff of L:.Teff /6R = (400 ::I:: 112) K kpc -1 and the logarithmic of the ionizing parameter log U ranging from -3.0 to -2.3. The N/O vs. O/H diagram derived from our results for isolated galaxies is in general consistent with chemical evolution models that assume that the nitrogen synthesis has both a primary and a secondary com¬ponent compared to oxygen. However, a very strong N/O dependence on the O/H at high abundances was found. Our models indicate that galaxies near to the core ofthe Virgo cluster are overabundant in O/H, N/O, and S/O by about 0.25 dex in comparison to the ones at the periphery. With one exception, models with upper stellar mass limit of Mu= 30-40 M0 and age of the ionizing star cluster ranging from 1.5 to 2.5 Myr were able to reproduce the observational data. Chemical evolution models indicate that the collapse time-scale for the inner regions of the galaxies near to the Virgo core is larger than the one in galaxies located at the intermediate and peripheral positions in the cluster, what can be due to the dense environment existing in the Virgo cluster core.Nós usamos modelos de fotoionização com o objetivo de derivar gradientes de abundâncias de O/H, N/O e S/O em três galáxias espirais barradas isoladas (NGC 1365, NGC 925, NGC 1073) e em nove galáxias espirais (NGC 4501, NGC 4571, NGC4689, NGC4254, NGC4321, NGC4654, NGC4303, NGC4651, NGC4713) no aglomerado de Virgem. Nossas predições para O/H mostraram-se consistentes com algumas determinações de abundância empíricas, mas elas estão superestimadas por um fator de 0.1-004 dex quando comparadas a medidas diretas de abundâncias. Para NGC 1365, nossos modelos não indicaram nenhuma quebra de gradientes, resultado sugerido por trabalhos anteriores. Em NGC 925, apesar do valor constante do in¬dicador de oxigênio R23 = ([O II]À3727+[0 III]À4949+À5007)/H,B para distâncias galactocêntricas R > 6.0 kpc, nossos modelos não mostraram nenhuma presença de quebra nos gradientes de abundâncias. NGC 1073 parece ser superabundante em nitrogênio comparada a outras espirais. Nenhum gradiente de S/O foi encon¬ trado nas galáxias estudadas, e nós derivamos um gradiente positivo na temperatura da estrela ionizante das nebulosas Teff de L.Teff / L.R = (400::f:: 112) K kpC-l e o parâmetro de ionização U variando de -3.0 < log U < -2.3. O diagrama de N/O vs. O/R derivado de nossos modelos para galáxias isoladas é consistente com mode¬los de evolução química que assumem que a síntese do nitrogênio tem componentes primários e secundários, em relação ao oxigênio. Entretanto, uma forte dependência de N/O com O/H a altas metalicidades foi encontrada. Nossos modelos indicam que galáxias próximas ao núcleo do aglomerado de Virgem são superabundantes em O/H, N/O e S/O por aproximadamente 0.25 dex em comparação àquelas localizadas na periferia. Com uma exceção, modelos com limites superiores de massa estelar de Mu= 30-40 M0 e idade do aglomerado ionizante de 1.5 a 2.5 milhões de anos foram capazes de reproduzir os dados observacionais. Modelos de evolução química indicam que a escala de tempo de colapso de regiões internas de galáxias próximas ao núcleo de Virgem é maior que o de galáxias localizadas nas posições intermediárias e periféricas do aglomerado, o que pode ser devido ao denso ambiente existente no núcleo desse aglomerado de galáxias.application/pdfporUniversidade Federal de Santa MariaPrograma de Pós-Graduação em FísicaUFSMBRFísicaFísicaPhysicsCNPQ::CIENCIAS EXATAS E DA TERRA::FISICAGradientes de abundâncias químicas em galáxias espiraisChemical gradients of abundâncias in galaxies spiralsinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/doctoralThesisCopetti, Marcus Vinicius Fontanahttp://lattes.cnpq.br/2566375872711558Schmidt, Alex Andrehttp://lattes.cnpq.br/4279165283013379Bergmann, Thaisa Storchihttp://lattes.cnpq.br/4999509031047259Lépine, Jacques Raymond Danielhttp://lattes.cnpq.br/9833768521859653Ludke, Evertonhttp://lattes.cnpq.br/8399842157129152http://lattes.cnpq.br/4238829381165820Dors Junior, Oli Luiz1005000000064003003003003003003000ff1515c-d729-47fe-826d-51e2734b9f5a15ae4920-9136-4911-aef8-0e6d926f5b0662bd98a3-43d6-4d56-846e-6e3de21c22690bac0e2a-57d9-4c79-bdc9-5d3922576ba7834bd13f-1acb-462d-969e-0c9c7c3fe2860ffafc58-49ad-4f2c-9c3d-d8b95c34464einfo:eu-repo/semantics/openAccessreponame:Manancial - Repositório Digital da UFSMinstname:Universidade Federal de Santa Maria (UFSM)instacron:UFSMORIGINALDissertacao de Oli.pdfapplication/pdf1386367http://repositorio.ufsm.br/bitstream/1/3939/1/Dissertacao%20de%20Oli.pdf6ed09b976ad22ef187a206108ecdabb8MD51TEXTDissertacao de Oli.pdf.txtDissertacao de Oli.pdf.txtExtracted texttext/plain412326http://repositorio.ufsm.br/bitstream/1/3939/2/Dissertacao%20de%20Oli.pdf.txt5b13c6e43e733589e9154a32910fc13dMD52THUMBNAILDissertacao de Oli.pdf.jpgDissertacao de Oli.pdf.jpgIM Thumbnailimage/jpeg5310http://repositorio.ufsm.br/bitstream/1/3939/3/Dissertacao%20de%20Oli.pdf.jpgdee4445a4543ee26df249f9341cecd5fMD531/39392023-01-05 10:09:39.339oai:repositorio.ufsm.br:1/3939Repositório Institucionalhttp://repositorio.ufsm.br/PUBhttp://repositorio.ufsm.br/oai/requestopendoar:39132023-01-05T13:09:39Manancial - Repositório Digital da UFSM - Universidade Federal de Santa Maria (UFSM)false |
dc.title.por.fl_str_mv |
Gradientes de abundâncias químicas em galáxias espirais |
dc.title.alternative.eng.fl_str_mv |
Chemical gradients of abundâncias in galaxies spirals |
title |
Gradientes de abundâncias químicas em galáxias espirais |
spellingShingle |
Gradientes de abundâncias químicas em galáxias espirais Dors Junior, Oli Luiz Física Physics CNPQ::CIENCIAS EXATAS E DA TERRA::FISICA |
title_short |
Gradientes de abundâncias químicas em galáxias espirais |
title_full |
Gradientes de abundâncias químicas em galáxias espirais |
title_fullStr |
Gradientes de abundâncias químicas em galáxias espirais |
title_full_unstemmed |
Gradientes de abundâncias químicas em galáxias espirais |
title_sort |
Gradientes de abundâncias químicas em galáxias espirais |
author |
Dors Junior, Oli Luiz |
author_facet |
Dors Junior, Oli Luiz |
author_role |
author |
dc.contributor.advisor1.fl_str_mv |
Copetti, Marcus Vinicius Fontana |
dc.contributor.advisor1Lattes.fl_str_mv |
http://lattes.cnpq.br/2566375872711558 |
dc.contributor.referee1.fl_str_mv |
Schmidt, Alex Andre |
dc.contributor.referee1Lattes.fl_str_mv |
http://lattes.cnpq.br/4279165283013379 |
dc.contributor.referee2.fl_str_mv |
Bergmann, Thaisa Storchi |
dc.contributor.referee2Lattes.fl_str_mv |
http://lattes.cnpq.br/4999509031047259 |
dc.contributor.referee3.fl_str_mv |
Lépine, Jacques Raymond Daniel |
dc.contributor.referee3Lattes.fl_str_mv |
http://lattes.cnpq.br/9833768521859653 |
dc.contributor.referee4.fl_str_mv |
Ludke, Everton |
dc.contributor.referee4Lattes.fl_str_mv |
http://lattes.cnpq.br/8399842157129152 |
dc.contributor.authorLattes.fl_str_mv |
http://lattes.cnpq.br/4238829381165820 |
dc.contributor.author.fl_str_mv |
Dors Junior, Oli Luiz |
contributor_str_mv |
Copetti, Marcus Vinicius Fontana Schmidt, Alex Andre Bergmann, Thaisa Storchi Lépine, Jacques Raymond Daniel Ludke, Everton |
dc.subject.por.fl_str_mv |
Física |
topic |
Física Physics CNPQ::CIENCIAS EXATAS E DA TERRA::FISICA |
dc.subject.eng.fl_str_mv |
Physics |
dc.subject.cnpq.fl_str_mv |
CNPQ::CIENCIAS EXATAS E DA TERRA::FISICA |
description |
We used photoionization models in order to derive O/H, N/O, and S/O abundance gradients in three isolated barred spiral galaxies (NGC 1365, NGC 925, NGC 1073) and in nine spiral galaxies (NGC 4501, NGC 4571, NGC 4689, NGC 4254, NGC4321, NGC4654, NGC4303, NGC4651, NGC4713) in the Virgo cluster. Our O/H predictions were found to be consistent with some empirical abundance de¬terminations, but are overestimated by a factor of 0.1-0.4 dex when compared to the direct abundance measures. For NGC 1365, our models indicate no abundance break, result suggested in previous works. ln NGC 925, despite the flattening in the R23 = ([O Il].\3727+[0 IlI].\4949+.\5007)/H,B oxygen indicator at galactocentric distances R > 6.0 kpc, our model results did not show any presence of an oxygen abundance break. NGC 1073 seems to be overabundant in nitrogen compared to other spiral galaxies. No gradient of S/O was found in the studied galaxies, and we derived a positive gradient for the ionizing star temperatures of the nebulae Teff of L:.Teff /6R = (400 ::I:: 112) K kpc -1 and the logarithmic of the ionizing parameter log U ranging from -3.0 to -2.3. The N/O vs. O/H diagram derived from our results for isolated galaxies is in general consistent with chemical evolution models that assume that the nitrogen synthesis has both a primary and a secondary com¬ponent compared to oxygen. However, a very strong N/O dependence on the O/H at high abundances was found. Our models indicate that galaxies near to the core ofthe Virgo cluster are overabundant in O/H, N/O, and S/O by about 0.25 dex in comparison to the ones at the periphery. With one exception, models with upper stellar mass limit of Mu= 30-40 M0 and age of the ionizing star cluster ranging from 1.5 to 2.5 Myr were able to reproduce the observational data. Chemical evolution models indicate that the collapse time-scale for the inner regions of the galaxies near to the Virgo core is larger than the one in galaxies located at the intermediate and peripheral positions in the cluster, what can be due to the dense environment existing in the Virgo cluster core. |
publishDate |
2006 |
dc.date.issued.fl_str_mv |
2006-06-28 |
dc.date.accessioned.fl_str_mv |
2017-05-09 |
dc.date.available.fl_str_mv |
2017-05-09 |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
dc.type.driver.fl_str_mv |
info:eu-repo/semantics/doctoralThesis |
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status_str |
publishedVersion |
dc.identifier.citation.fl_str_mv |
DORS JUNIOR, Oli Luiz. Chemical gradients of abundâncias in galaxies spirals. 2006. 111 f. Tese (Doutorado em Física) - Universidade Federal de Santa Maria, Santa Maria, 2006. |
dc.identifier.uri.fl_str_mv |
http://repositorio.ufsm.br/handle/1/3939 |
identifier_str_mv |
DORS JUNIOR, Oli Luiz. Chemical gradients of abundâncias in galaxies spirals. 2006. 111 f. Tese (Doutorado em Física) - Universidade Federal de Santa Maria, Santa Maria, 2006. |
url |
http://repositorio.ufsm.br/handle/1/3939 |
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por |
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