Submitted by Automa??o e Estat?stica (sst@bczm.ufrn.br) on 2016-07-25T21:57:03Z No. of bitstreams: 1 IcaroKennedyFrancelinoMoura_DISSERT.pdf: 6308092 bytes, checksum: 65c9e0d99b3ea645902b37237e873ed1 (MD5) / Approved for entry into archive by Arlan Eloi Leite Silva (eloihistoriador@yahoo.com.br) on 2016-08-03T20:32:51Z (GMT) No. of bitstreams: 1 IcaroKennedyFrancelinoMoura_DISSERT.pdf: 6308092 bytes, checksum: 65c9e0d99b3ea645902b37237e873ed1 (MD5) / Made available in DSpace on 2016-08-03T20:32:51Z (GMT). No. of bitstreams: 1 IcaroKennedyFrancelinoMoura_DISSERT.pdf: 6308092 bytes, checksum: 65c9e0d99b3ea645902b37237e873ed1 (MD5) Previous issue date: 2016-03-02 / Coordena??o de Aperfei?oamento de Pessoal de N?vel Superior (CAPES) / Grandes esfor?os observacionais t?m sido direcionados para investigar a natureza da chamada energia escura. Nesta disserta??o derivamos v?nculos sobre modelos de energia escura utilizando tr?s diferentes observ?veis: medidas da taxa de expans?o H(z) (compiladas por Meng et al. em 2015); m?dulo de dist?ncia de 580 Supernovas do Tipo Ia (cat?logo Union Compilation 2.1, 2011); e as observa??es do pico de oscila??o de b?rions (BAO) e a radia??o c?smica de fundo (CMB) utilizando a chamada raz?o CMB/BAO, que relaciona 6 picos de BAO (um pico determinado atrav?s dos dados do Survey 6dFGS, dois atrav?s do SDSS e tr?s atrav?s do WiggleZ). A an?lise estat?stica utilizada foi o m?todo do ?2 m?nimo (marginalizado ou minimizado sobre h sempre que poss?vel) para vincular os par?metro cosmol?gicos: ?m, ??, ? e ??0. Esses testes foram aplicados em duas parametriza??es do par?metro ? da equa??o de estado da energia escura, p=?? (aqui, p ? a press?o e ? ? a densidade de energia da componente). Numa, ? ? considerado constante e menor que -1/3, conhecido como modelo XCDM; na outra parametriza??o, o par?metro da equa??o de estado varia com o redshift, no qual o chamamos de Modelo GS. Esta ?ltima parametriza??o ? baseada em argumentos que surgem da teoria da infla??o cosmol?gica. Para efeitos de compara??o tamb?m foi feita a an?lise do modelo ?CDM. A compara??o dos modelos cosmol?gicos com as diferentes observa??es leva a diferentes melhores ajustes. Assim, para classificar a viabilidade observacional dos diferentes modelos te?ricos, utilizamos dois crit?rios de informa??o, ou seja, o crit?rio de informa??o bayesiana (BIC) e o crit?rio de informa??o Akaike (AIC). A ferramenta matriz de Fisher foi incorporada aos nossos testes para nos fornecer a incerteza dos par?metros de cada modelo te?rico. Verificamos que a complementariedade dos testes ? necess?ria para n?o termos espa?os param?tricos degenerados. Fazendo o processo de minimiza??o encontramos, dentro da regi?o de 1? (68%), que para o Modelo XCDM os melhores ajustes dos par?metros s?o ?m=0,28?0,012 e ?X=-1,01?0,052. Enquanto que para o Modelo GS os melhores ajustes s?o ?m=0,28?0,011 e ??0=0,00?0,059. E realizando uma marginaliza??o encontramos, dentro da regi?o de 1? (68%), que para o Modelo XCDM os melhores ajustes dos par?metros s?o ?m=0,28?0,012 e ?X=-1,01?0,052. Enquanto que para o Modelo GS os melhores ajustes s?o ?m=0,28?0,011 e ??0=0,00?0,059. / A significant observational effort has been directed to investigate the nature of the so-called dark energy. In this dissertation we derive constraints on dark energy models using three different observable: measurements of the Hubble rate H(z) (compiled by Meng et al. in 2015.); distance modulus of 580 Supernovae Type Ia (Union catalog Compilation 2.1, 2011); and the observations of baryon acoustic oscilations (BAO) and the cosmic microwave background (CMB) by using the so-called CMB/BAO of six peaks of BAO (a peak determined through the Survey 6dFGS data, two through the SDSS and three through WiggleZ). The statistical analysis used was the method of the ?2 minimum (marginalized or minimized over h whenever possible) to link the cosmological parameter: m, ? and ??0. These tests were applied in two parameterization of the parameter ? of the equation of state of dark energy, p = ?? (here, p is the pressure and ? is the component of energy density). In one, ? is considered constant and less than -1/3, known as XCDM model; in the other the parameter of state equantion varies with the redshift, where we the call model GS. This last model is based on arguments that arise from the theory of cosmological inflation. For comparison it was also made the analysis of model CDM. Comparison of cosmological models with different observations lead to different optimal settings. Thus, to classify the observational viability of different theoretical models we use two criteria information, the Bayesian information criterion (BIC) and the Akaike information criteria (AIC). The Fisher matrix tool was incorporated into our testing to provide us with the uncertainty of the parameters of each theoretical model. We found that the complementarity of tests is necessary inorder we do not have degenerate parametric spaces. Making the minimization process we found (68%), for the Model XCDM the best fit parameters are m = 0.28 ? 0, 012 and ?X = ?1.01 ? 0, 052. While for Model GS the best settings are m = 0.28 ? 0, 011 and ??0 = 0.00 ? 0, 059. Performing a marginalization we found (68%), for the Model XCDM the best fit parameters are m = 0.28 ? 0, 012 and ?X = ?1.01 ? 0, 052. While for Model GS the best settings are M = 0.28 ? 0, 011 and ??0 = 0.00 ? 0, 059.

Die Messung der dunklen Energie Ω(Λ) und des equation-of-state Parameters 𝑤 spielen in der Kosmologie eine entscheidende Rolle. Das Hubble-Diagramm einer Supernova vom Typ Ia (SNe-Ia) gibt Aufschluss über diese Parameter. Die Supernova-Kosmologie vergleicht die Lichtkurven von SNe-Ia bei verschiedenen Rotverschiebungen und Filterbändern. Die Genauigkeit der oben genannten Parameter hängt von der Genauigkeit der derzeit verfügbaren spektrophotometrischen Standards ab. Dies erfordert Fortschritte bei der Verbesserung der Verbindung zwischen den derzeitigen astrophysikalischen Flussstandards und den in den Labors etablierten Standards. CALSPEC ist ein stellares Standardnetzwerk mit einer internen Konsistenz von 0,5 %, das häufig mit STIS am Hubble-Weltraumteleskop validiert wird. Neue Instrumente wie das Vera C. Rubin-Observatorium erfordern Flusskalibrierungsunsicherheiten in der Größenordnung von 0,1 %. SCALA zielt darauf ab, die Kalibrierung des NIST-Laborstandards mit Unsicherheiten, die von den NIST-Kalibrierungsunsicherheiten dominiert werden, auf CALSPEC zu übertragen. SCALA verwendet zwei sequentielle Monochromatoren zur gleichzeitigen Beleuchtung des SNIFS+Teleskopsystems. Zwanzig Photosensoren wurden kalibriert für den Bereich zwischen 3000Å und 10 000 Å, und SCALA wurde im Juni 2022 mit den vorgeschlagenen Verbesserungen aufgerüstet. Nach Abschluss der Aufrüstung wurden in vier Nächten zwischen dem 19. und 22. Juni 2022 Standardsterne aus dem von der Supernova Factory verwendeten Standardsternnetz beobachtet. Tagsüber wurde SNIFS anhand der zuvor kalibrierten Fotosensoren kalibriert, so dass die Kalibrierung auf den NIST-Laborstandard zurückgeführt werden konnte. Es zeigte sich, dass der Kalibrierungstransfer von SCALA in der Größenordnung von 0,1 % zum gesamten Unsicherheitsbudget beiträgt. Eine Anpassung der SNIFS-Analysepipeline wird den Vergleich mit CALSPEC mit Unsicherheiten von weniger als 0,5 % ermöglichen. / The measurement of dark energy Ω(Λ) and its equation of state parameter 𝑤 plays a vital role in cosmology. The Hubble diagram of a Type Ia supernova (SNe-Ia) constrains these parameters. Supernova cosmology compares the light curves of SNe-Ia at different redshifts and filter bands. The accuracy of the above parameters depends on the accuracy of currently available spectrophotometric standards. This requires advances to improve the connection between current astrophysical flux standards and those established in laboratories. CALSPEC is a standard stellar network with an internal consistency of 0.5%, frequently validated with STIS at the Hubble Space Telescope. New instruments such as the Vera C. Rubin Observatory require flux calibration uncertainties of the order of 0.1%. SCALA aims to transfer the calibration of the NIST laboratory standard with uncertainties dominated by the NIST calibration uncertainties to CALSPEC. SCALA uses two sequential monochromators to simultaneously illuminate the SNIFS + telescope system and the calibrated photodiodes with traceable calibration for the range between 3000Å to 10 000 Å. Twenty photosensors were calibrated, and SCALA was upgraded with the proposed improvements in June 2022. At the end of the upgrade, standard stars from the standard star network used by the Supernova Factory were observed for four nights between June 19 and 22, 2022. During the day, SNIFS was calibrated against the previously calibrated photosensors, allowing the calibration to be traced back to the NIST laboratory standard. It was shown that the calibration transfer from SCALA contributes in the order of 0.1%to the total uncertainty budget. An adjustment of the SNIFS analysis pipeline will allow comparison with CALSPEC with uncertainties less than 0.5%.

Made available in DSpace on 2014-12-17T15:15:02Z (GMT). No. of bitstreams: 1 HumbertoSG_DISSERT.pdf: 1623099 bytes, checksum: 9db2624a800c722b68b561bc7a9bc747 (MD5) Previous issue date: 2013-04-01 / Coordena??o de Aperfei?oamento de Pessoal de N?vel Superior / Nesta disserta??o, uma revis?o sobre tr?s modelos cosmol?gicos n?o-padr?o do tipo Friedmann-Robertson-Walker s?o apresentados. O modelo !CDM, o g?s de Chaplygin generalizado e o modelo de brana de Dvali-Gabadadze-Porrati (DGP). Apresentamos tamb?m, tr?s testes estat?sticos utilizados em Cosmologia, cada um envolvendo uma vela padr?o diferente. Estes testes t?m como objetivo, vincular os diferentes par?metros de cada modelo e assim compar?-los com os dados observacionais mais atuais. Efetuamos o teste do m?dulo de dist?ncia de Supernovas do tipo Ia, atrav?s de 580 Supernovas do Union Compilation 2.1 (2011) [1]. A Fra??o de massa de aglomerados de gal?xias, onde utilizamos um conjunto de 52 aglomerados observados pelo CHANDRA (2009) [2] e a raz?o CMB/BAO, onde foram utilizados um conjunto de 6 picos de BAO do WiggleZ Dark Energy Survey (2011) [3]. Esses testes foram aplicados para cada um dos modelos apresentados. Verificamos que individualmente, os testes cosmol?gicos n?o s?o bons o suficiente para vincular modelos, criando espa?os param?tricos degenerados, necessitando de uma an?lise em conjunta dos testes para vincular os par?metros. OBS: N?o foi poss?vel efetuar a descri??o integral do resumo, devido o fato do sistema utilizado n?o aceitar os s?mbolos existentes. Desse modo, solicitamos que a visualiza??o desse elemento seja efetuada no arquivo da disserta??o.