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UNIVERSIDADE FEDERAL DE SANTA CATARINA Centro De Ciências Físicas E Matemáticas – CFM Fábio Rafael Herpich PLANO DE APOSEN

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UNIVERSIDADE FEDERAL DE SANTA CATARINA Centro De Ciências Físicas E Matemáticas – CFM Fábio Rafael Herpich PLANO DE APOSEN UNIVERSIDADE FEDERAL DE SANTA CATARINA Centro de Ciências Físicas e Matemáticas – CFM Fábio Rafael Herpich PLANO DE APOSENTADORIA GALÁCTICA: Galáxias Early-type do Ultravioleta ao Infravermelho Florianópolis (SC) 2017 Fábio Rafael Herpich PLANO DE APOSENTADORIA GALÁCTICA: Galáxias Early-type do Ultravioleta ao Infravermelho∗ Trabalho realizado sob orientação do Prof. Dr. Roberto Cid Fernandes e co- orientação do Prof. Dr. Abílio Mateus apresentado ao Departamento de Física da UFSC em preenchimento aos requisitos da investidura ao título de Doutor em Física. Florianópolis (SC) 2017 ∗ Trabalho financiado pelas agências de fomento FAPESC e CAPES. Ficha de identificação da obra elaborada pelo autor, através do Programa de Geração Automática da Biblioteca Universitária da UFSC. Herpich, Fábio Rafael Plano de Aposentadoria Galáctica : Galáxias early-type do ultravioleta ao infravermelho / Fábio Rafael Herpich ; orientador, Roberto Cid Fernandes ; coorientador, Abílio Mateus. - Florianópolis, SC, 2017. 149 p. Tese (doutorado) - Universidade Federal de Santa Catarina, Centro de Ciências Físicas e Matemáticas. Programa de Pós-Graduação em Física. Inclui referências 1. Física. 2. galáxias. 3. astronomia extragaláctica. 4. galáxias early-type. 5. populações estelares. I. Cid Fernandes, Roberto. II. Mateus, Abílio. III. Universidade Federal de Santa Catarina. Programa de Pós-Graduação em Física. IV. Título. AGRADECIMENTOS • Aos professores Abílio Mateus, Roberto Cid Fernandes, Natalia Vale Asari e Grazyna Stasińska pelas orientações e parceria, sem as quais certamente este trabalho não existiria; • Ao professor Antonio Kanaan, pelos valiosos ensinamentos, tanto profissionais quanto pessoais; • Ao professor Raymundo Baptista, pela primeira oportunidade e pri- meiros passos na Astronomia; • Aos meus pais, D. Vanderli e S. Adenor, e meus irmãos Marcio, Jona- tas e Zuleica, pelo apoio ininterrupto em minha vontade de estudar frente às dificuldades encontradas ao longo do caminho trilhado; • À Morgana pelo companheirismo e afeto dispensado nos momentos bons e pela paciência nos ruins; • Aos amigos do Grupo de Astrofísica da UFSC (GAS-UFSC) Saito, Bernardo, Tiago (hoje professores) William e Lacerda pelo grande auxílio nas fases iniciais, especialmente com o “obscuro” Linux e com a programação; • Aos amigos e colegas do GAS (ou não) que estiveram presentes de alguma forma nas atividades, dando suas opiniões ou, simplesmente, ouvindo as (muitas) reclamações; • Aos meus caros amigos da Jamaitemática, pelas horas de descontra- ção, parceria e ajuda na degustação dos derivados da cevada; • A todos os amigos e pessoas que de um modo ou de outro participam ou participaram do dia a dia desta universidade. A todos, muito obrigado! “(. ) O Primeiro Orador já acabara há muito tempo de falar com o estudante. Fora, na verdade, uma exposição para si mesmo, ali, de pé diante da janela, enquanto levantava os olhos para o espelendor incrível do firmamento, para a imensa Galáxia que estava agora segura para sempre.” (Asimov, 1976, pg. 503) RESUMO O paradigma da classificação espectral de galáxias, largamente utilizado atualmente com o avanço das técnicas de síntese espectral, dos modelos de populações estelares e dos grandes levantamentos de dados, proporcio- nou a obtenção de uma quantidade sem precedentes de informações físicas acerca da evolução das galáxias no Universo. Neste contexto, utilizamos dados públicos de três grandes levantamentos de galáxias, cobrindo desde o ultravioleta (Galaxy Evolution Explorer; GALEX), passando pelo óptico (Sloan Digital Sky Survey; SDSS), até o infravermelho médio (Wide-field Infrared Survey Explorer; WISE), com o objetivo de investigar as propri- edades de galáxias early-type classificadas com base nas linhas de emissão presentes ou ausentes em seus espectros. Investigamos as propriedades físicas no WISE da classe de galáxias hospe- deiras de região de emissão nuclear de baixa ionização (LINER), definidas por meio de diagramas de diagnóstico de linhas de emissão. Neste pro- cesso, utilizamos as classes espectrais definidas através do método que leva em consideração a largura equivalente de Hα e a razão [N ii]/Hα, obtendo uma linha divisória “ideal” que separa as galáxias do Universo Local entre as que são puramente star forming daquelas que já estão “aposentadas” da tarefa de formar estrelas. Utilizando os indicadores morfológicos disponibi- lizados pelo Galaxy Zoo, percebemos que ∼ 30% das galáxias classificadas como aposentadas são objetos espirais, com disco extenso dominado por regiões de formação estelar. Nestes objetos, a fibra utilizada na obtenção do espectro utilizado na classificação espectral observou apenas a região do bojo dominada por populações estelares velhas. Com estes apontamentos, selecionamos uma amostra de LINERs utilizando diferentes marcadores, de forma a testar se de fato possuem núcleo ativo (AGN) quando considerado um combinado de linhas de emissão com a cor no infravermelho. Encon- tramos que a maior parte destas galáxias não hospedam de fato um AGN, com suas linhas de emissão sendo providas pelas populações de estrelas evoluídas de baixa massa (HOLMES). Excluída a contribuição de AGN, investigamos as propriedades das ga- láxias “aposentadas”, cuja característica é a ausência de formação estelar recente quantificada pela largura equivalente de Hα, WHα. Estes obje- tos pararam de formar estrelas há muito tempo e seus espectros mostram somente contribuições de estrelas velhas. São divididas em duas classes: (1) galáxias que possuem linhas de emissão fracas, com 0;5 < WHα < 3 Å (ELR); e (2) galáxias sem linhas, com WHα < 0;5 Å (LLR). Utilizando os fluxos no infravermelho médio do WISE, observamos que as ELR são mais brilhantes na banda centrada em torno de 12 µm, associada com emissão oriunda de poeira morna. Em uma comparação com os dados obtidos com a síntese espectral com o código Starlight, percebemos que estas duas classes de galáxias aposentadas também têm atenuação (AV ) diferente, com características similares às da emissão em 12 µm. Isto indica que a luz emitida pelas estrelas velhas é reprocessada por um meio difuso. Com- parando galáxias similares das duas classes, não encontramos evidências de outras diferenças significativas nas propriedades de suas populações es- telares, especialmente nas idades médias. Porém, análises comparativas envolvendo emissão no ultravioleta e indicadores de idade e metalicidade mostram que a metalicidade das duas classes tem uma diferença sensível, enquanto que a idade das populações estelares é sistematicamente dife- rente, com as ELR sendo um pouco mais jovens. Desta forma, isto implica na coexistência dos dois fenômenos: presença de gás difuso e populações estelares com idades diferentes. Neste sentido, sugerimos um cenário em −1 que alguma formação estelar (SF R < 0;3 M yr ) tenha ocorrido em um tempo entre 1 e 5 Gyr nas ELR através da adição de material frio do meio externo. Nas galáxias LLR, este fenômeno parou em um tempo muito maior (t > 5 Gyr), de forma que apenas são observadas as popula- ções estelares velhas. Neste caso, nas ELRs é observada uma mistura de propriedades físicas, compostas pela parte oriunda das propriedades das estrelas velhas e pela contribuição das mais jovens. Neste cenário, a pre- sença de um meio interestelar difuso também é compatível, uma vez que o material adquirido ainda não dissipou completamente, estando espalhado nas partes externas da galáxia. Palavras-chave: galáxias; astronomia extragaláctica; galáxias early-type; populações estelares ABSTRACT The galaxy spectral classification paradigm, largely used nowadays with the advance of the spectral synthesis techniques, the stellar population models and the large galaxy surveys, have allowed us the acquisition of a huge amount of physical properties of galaxies in the Universe. In this way, we use the data of three public surveys, covering from the ultraviolet (Galaxy Evolution Explorer; GALEX), passing through the optic (The Sloan Digital Sky Survey; SDSS), and reaching the mid-infrared (Wide- field Infrared Survey; WISE), with the aim to investigate the properties of early-type galaxies classified based on the presence or absence of emission lines in their spectra. Initially, we investigate the mid-infrared properties of galaxies hosting a low ionization nuclear emission region (LINER), defined by emission line diagnostic diagrams. We use the spectral classes defined by the method that take into account the equivalent width of Hα and the [N ii]/Hα ratio, obtaining an optimal divisor line which separate star forming galaxies from galaxies that are retired from their duty of forming stars. Selecting these galaxies using the morphological information from the Galaxy Zoo project, we realize that many of the retired galaxies have spiral morphology, with only the old bulge being observed by the SDSS fiber. We then select a sample of LINERs using different definitions to test if they are in fact hosting an active nuclei (AGN) when considering a combination of emission lines and infrared colors. We find that most of these objects are not truly AGN, but their emission lines are powered by their hot low-mass stellar populations (HOLMES). Excluded the AGN contribution, we investigate the properties of retired galaxies, characterized by the absence of recent star formation as quanti- fied by the equivalent width of Hα, WHα. These objects stopped forming stars long ago and their spectra show only the contribution of old stel- lar populations. These galaxies are divided into two classes: (1) galaxies
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