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Espectroscopia IFU Das Galáxias “Seyfert/Starburst” NGC 6221 E

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Espectroscopia IFU Das Galáxias “Seyfert/Starburst” NGC 6221 E Universidade de S˜aoPaulo Instituto de Astronomia, Geof´ısicae CiˆenciasAtmosf´ericas Departamento de Astronomia Tiago Vecchi Ricci Espectroscopia IFU das gal´axias “Seyfert/starburst” NGC 6221 e NGC 7582 S˜aoPaulo 2008 Tiago Vecchi Ricci Espectroscopia IFU das gal´axias “Seyfert/starburst” NGC 6221 e NGC 7582 Disserta¸c˜aoapresentada ao Departamento de Astronomia do Instituto de Astronomia, Geof´ısicae CiˆenciasAtmosf´ericas da Universidade de S˜aoPaulo como parte dos requisitos para a obten¸c˜aodo t´ıtulode Mestre em Ciˆencias. Area´ de Concentra¸c˜ao:Astronomia Orientador: Prof. Dr. Jo˜aoEvangelista Steiner S˜aoPaulo 2008 Ao meu pai Douglas e minha m˜aeNadir. Agradecimentos Gostaria de agradecer primeiramente `aminha fam´ılia(meus pais Douglas e Nadir, meus irm˜aosErico e Bruno, minha cunhada Heydde, minha sobrinha Larissa, meus avˆosIvo e Francisco e minhas av´osIrene e Elvira) por sempre estarem ao meu lado. Agrade¸comeu orientador Jo˜aoEvangelista Steiner por ajudar a construir o caminho de meu conhecimento na astronomia que vem desde a inicia¸c˜aocient´ıficae que continuar´a a ser trilhado durante o doutorado. A` Roberto Cid Fernandes, pela ajuda com o programa “Starlight” e por coment´arios importantes sobre as gal´axiasalvo dessa disserta¸c˜aoe `a Aurea´ Garcia-Rissmann por permi- tir a utiliza¸c˜aodos dados analisados nesta disserta¸c˜ao.Agrade¸cotamb´em`aLaerte Sodr´e Jr. pelos coment´ariosnos relat´oriosdo departamento. A` Alexandre Soares de Oliveira pelas in´umerasajudas principalmente na redu¸c˜aode dados do Gemini. Agrade¸cotamb´em meu colega Roberto Menezes pelas ajudas sempre importantes no desenvolvimento do tra- balho. E um grande agradecimento ao Raimundo Lopes de Oliveira pela paciˆenciaque ele teve em ler a primeira vers˜aode minha disserta¸c˜ao,o que n˜aodeve ter sido nada agrad´avel. A` F´atimae ao Aziz do IEA, ambos sempre me deram uma m˜aonas horas certas. Aos bons amigos que fiz durante a p´os-gradua¸c˜ao:Patr´ıciaCruz, Rodrigo Vieira, Os- caaaaaaaaaaaaaaaaaaar (o cara mais peligroso do IAG), Felipe Santos, Marcio Avelar, Marcio Barreto, S´ergio(gringo), Grazi, Tatiana Lagan´a,Z´eColm´eia(esse j´a´edo tempo da gradua¸c˜ao)e bem, ao Pedro Paulo tamb´em. E a todos os colegas do IAG que me ajudaram durante esses dois anos do mestrado. Agrade¸coa FAPESP, pelo apoio financeiro, sob o projeto no 2005/03323-9. “And in the end, the love you take is equal to the love you make” Lennon/McCartney “A mente que se abre a uma nova id´eiajamais voltar´aao seu tamanho original” Albert Einstein Resumo Gal´axias Seyfert s˜aoassociados a objetos com presen¸cade atividade nuclear (AGN, de “active galatic nuclei”). Seus espectros no ´opticopossuem linhas em emiss˜aopermitidas e proibidas e s˜aomais alargadas em rela¸c˜ao`aslinhas observadas em “starbursts” ou em nebulosas planet´arias,indicando um g´asde baixa densidade rotacionando em torno de 6−9 um objeto massivo, provavelmente um buraco negro com massa na faixa de 10 M¯. As gal´axiasSeyfert s˜aodivididas em tipo 1 (presen¸cade asas largas nas linhas permitidas) e tipo 2 (ausˆenciade asas largas nas linhas permitidas). NGC 6221 e NGC 7582 s˜aogal´axias cujos espectros na faixa do ´opticos˜aocaracter´ısticosde regi˜oesH II. Por´em,as linhas de [O III]λ4959,5007A˙ sugerem a presen¸cade uma Seyfert 2 e os espectros em raio-x s˜ao peculiares a uma Seyfert 1. Atrav´esda espectroscopia de campo integral (IFU), estudamos as propriedades dessas gal´axias“Seyfert/starburst”. Neste trabalho utilizamos a t´ecnicada tomografia PCA. Para uma an´alisemais precisa, fizemos um estudo sobre deconvolu¸c˜aode imagens atrav´esdo m´etodo de Richardson-Lucy. Apresentamos um m´etodo de corre¸c˜aodo efeito da refra¸c˜ao atmosf´ericaem cubo de dados, onde revisamos teorias sobre este efeito. Na gal´axiaNGC 6221, a an´alisecom o PCA revelou a presen¸cade duas regi˜oesH II, dois “clusters” de estrelas do tipo Wolf-Rayet (WR) e restos de supernovas, observados principalmente na linha de [N I]λ5198A˙ e He II. Esta gal´axiapossui um pico duplo nas linhas de [O III]λ4959,5007A˙, que, junto com as imagens referentes a cada pico de [O III], revela a presen¸cade uma atividade nuclear dupla, talvez o resultado mais surpreendente deste trabalho. Em NGC 7582, a an´alisecom o PCA mostrou tamb´ema presen¸cade duas regi˜oesH II, o AGN e restos de supernovas. Analisamos, ainda, uma amostra de gal´axiasSeyfert pr´oximas;mostramos que a va- rian¸ca´edominada pela taxa de acre¸c˜aode mat´eriano buraco negro. A segunda componente ´eexplicada pela massa do buraco negro central, revelando um efeito de “downsizing” no universo local, dada a correla¸c˜aoda massa do bojo da gal´axia,que ´eproporcional a massa do buraco negro, com a atividade nuclear e a anticorrela¸c˜aoentre a massa e a presen¸cade regi˜oesde forma¸c˜aoestelar. O desenvolvimento da metodologia apresentada nesta disserta¸c˜aofoi testada e aper- fei¸coadaao longo do mestrado. Com ela, conseguimos revelar caracter´ısticasimportantes nas gal´axiasNGC 6221 e NGC 7582, como a presen¸cade restos de supernovas, de duas regi˜oesH II em cada gal´axiae a localiza¸c˜ao,bem como a caracteriza¸c˜ao,de seus AGNs. Abstract Seyfert Galaxies are associated to objects having nuclear activity (AGN, from “active galatic nuclei”). Their spectra in the optical have permited and forbidden emission lines and they are broader than those observed in starbursts or in planetary nebulae, indicating low density gas rotating around a massive object, probably a black hole with mass in 6−9 the range of 10 M¯. Seyfert galaxies are divided in type 1 (presence of broad wings in permitted lines) and type 2 (absence of broad wings in permitted lines). NGC 6221 and NGC 7582 are galaxies whose optical spectra have characteristics of H II regions. However, [O III]λ4959,5007A˙ lines suggest the presence of a Seyfert 2 and the x-ray spectra are similar to Seyfert 1. We studied the properties of these Seyfert/staburst galaxies with the integral field spectroscopy (IFU). In this work, we used the PCA tomography technique. To improve the analysis, we made the image deconvolution using the Richardson-Lucy method. We present a way of correcting the effect of atmospheric refraction in datacubes. In NGC 6221, the PCA analisys revealed the presence of two H II regions, two clusters of Wolf-Rayet (WR) stars and supernovae remnants, observed mainly in the [N I]λ5198A˙ and He II. This galaxy has a double-peaked profile in [O III]λ4959,5007A˙ lines that, together with the images referent to each peak of [O III], shows a double nuclear activity. In NGC 7582, the PCA tomography showed also the presence of two H II regions, the AGN and supernovae remnants. In addition, we analysed a sample of near Seyfert galaxies; we showed that the variance is dominated by the acretion rate of matter into the black hole. The second component is explained by the central black hole mass, revealing a downsizing effect in the local universe, given the correlation between the galaxy’s bulge mass, which is proportional to the black hole mass, with the nuclear activity and the anti-correlation between this mass and the presence of starburst regions. The development of the methodoly presented in this dissertation was tested and im- proved throught the master course. With it, we were able to show important features in NGC 6221 and NGC 7582 galaxies, like the presence of supernovae remnants, two H II regions in each galaxy and the location as well as the characterization of their AGNs. Lista de Figuras 1.1 Esquema conceitual para a unifica¸c˜aoentre as Sy1 e Sy2. Um toro de poeira esconde a fonte do cont´ınuo (ponto preto no centro) e a BLR (nuvens perto do centro). No entanto, as NLR est˜aofora do toro, por isso apenas as linhas estreitas s˜aoobservadas nas Sy2. No eixo do toro, o n´ucleon˜ao´eobstru´ıdo e a mesma gal´axia´eclassificada como Sy1. Figura de Peterson (1997) . 31 1.2 Espectro de NGC 1068. O espectro acima n˜ao´epolarizado e possui apenas linhas estreitas. O espectro abaixo, polarizado, apresenta evidˆenciasde linhas permitidas largas, indicando que a gal´axia´euma Sy1 intr´ınseca. Figura de Osterbrock e Ferland (2006) . 32 1.3 Observa¸c˜aoda fonte H1649-595. Caixas de erro com tamanhos 3.60 e 0.84 em graus2. O asterisco ´ea posi¸c˜aoda poss´ıvel fonte, no caso NGC 6221. Figura de Marshall et al. (1979) . 35 1.4 Espectro de NGC 6221, de Veron et al. (1981). As linhas em emiss˜aode [O III] s˜aoclaramente mais largas que Hβ. Figura de Veron et al. (1981) . 35 1.5 Compara¸c˜aoentre os perfis de linhas de [O III] e Hβ. Est˜aoplotadas na mesma escala de velocidade relativa `avelocidade m´edianuclear. Figura de Pence e Blackman (1984) . 36 1.6 Raz˜aodas linhas nucleares de [O III]λ5007A e as linhas de Hβ da figura 1.5. A raz˜aovaria no pico de aproximadamente 0.2 correspondem a regi˜oesHII at´eaproximadamente 3 na asa azul indicando uma Sy2. Figura de Pence e Blackman (1984) . 36 1.7 Esquematiza¸c˜aodo modelo de “starburst” obscurecendo o AGN. A linha de visada A ´eo que acontece com NGC 6221, onde a BLR e a NLR s˜ao escondidas pelo “starburst”. Como a coluna de densidade do AGN medido no raio-x ´eda ordem de 1022cm−2, as caracter´ısticasde Sy1 nesta faixa do espectro n˜ao´euma surpresa.
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