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Elmufti, Mohammed. "Perturbations of dark energy models." Thesis, University of Western Cape, 2012. http://hdl.handle.net/11394/3386.
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>Magister Scientiae - MScThe growth of structure in the Universe proceeds via the collapse of dark matter and baryons. This process is retarded by dark energy which drives an accelerated expansion of the late Universe. In this thesis we use cosmological perturbation theory to investigate structure formation for a particular class of dark energy models, i.e. interacting dark energy models. In these models there is a non-gravitational interaction between dark energy and dark matter, which alters the standard evolution (with non-interacting dark energy) of the Universe. We consider a simple form of the interaction where the energy exchange in the background is proportional to the dark energy density. We analyse the background dynamics to uncover the e ect of the interaction. Then we develop the perturbation equations that govern the evolution of density perturbations, peculiar velocities and the gravitational potential. We carefully account for the complex nature of the perturbed interaction, in particular for the momentum transfer in the dark sector. This leads to two di erent types of model, where the momentum exchange vanishes either in the dark matter rest-frame or the dark energy rest-frame. The evolution equations for the perturbations are solved numerically, to show how structure formation is altered by the interaction.
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Duran, Sancho Ivan. "Constraining Cosmological Models of Dark Energy." Doctoral thesis, Universitat Autònoma de Barcelona, 2013. http://hdl.handle.net/10803/125917.
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Avui en dia, l'Univers sembla estar experimentant una fase d'expansió accelerada, com ho demostren les dades de supernoves i posteriorment corroborada per una sèrie de mesuraments cosmològiques -molt recentment pel satèl·lit Planck. Mentre que aquesta expansió pot ser descrit en la teoria de la gravetat d'Einstein mitjançant la invocació de l'existència d'una positiva, però extremadament petita constant cosmològica, Λ, connectat al buit quàntic, s'han proposat moltes alternatives. A grans trets, el contingut d'energia de l'univers actual es pot dividir en 5% de la matèria bariònica i el 95% d'un invisible (conegut com el "sector fosc", perquè els seus components no interactuen electromagnèticament), el 25% del qual constituït per matèria no-relativista, partícules massives d'interacció feble ("matèria fosca freda") i un 75% d'un component amb una enorme pressió negativa, l'anomenada "energia fosca". La naturalesa d'aquest últim component és completament desconegut, això justifica que s'han proposat molts candidats "de prova". De moment, la més simple i de més èxit és la constant cosmològica, esmentada anteriorment. No obstant això, pateix de dos inconvenients principals a nivell teòric: el problema de la coincidència i el problema del “fine-tunning”. L'objectiu d'aquesta memòria és proposar i ajustar els models cosmològics de l'energia fosca que eviten aquestes dificultats.
Aquesta tesi està organitzada de la següent manera: Els capítols § 2, § 3 i § 4 s'introdueixen conceptes bàsics utilitzats en considerar els diferents models que conformen el nostre treball de recerca. Els següents capítols se centren en els diferents models cosmològics. Al § 5, l'energia fosca compleix el principi hologràfic i es postula que interactua (també sense gravetat) amb la matèria fosca. El principi hologràfic estableix una escala de longitud, en aquest cas la longitud d' Hubble, és a dir, la distància que limita els esdeveniments causalment connectats. Al capítol § 6, s'estudia amb més profunditat el model anterior, i es presenta una alternativa al mateix. Tots dos models comparteixen l'evolució fons idèntica però cada component es comporta de manera diferent, la qual cosa indueix un comportament divers quan es consideren les pertorbacions. Això permet discriminar observacionalment un model de l'altre.
Un model d'energia fosca hologràfica més es proposa en el § 7, aquest amb l’escala de longitud determinada per el Radi de Ricci (és a dir, la mida màxima d'una pertorbació que condueix a un forat negre). Un cop més, es suposa una interacció no-gravitacional entre l'energia fosca i la matèria fosca. Al § 8, s'estudia un model unificat (amb una unificació entre la matèria fosca ad energia fosca) proposat anteriorment. Atès que l'espai de paràmetres que s'ajusta a les dades observacionals és molt petit (i també en vista del seu interès teòric), descomponem el component únic en matèria fosca freda i buit que interactuen entre ells. Com a conseqüència, l'espai de paràmetres permesos queda augmentada considerablement. Encara que els models esmentats anteriorment imiten a nivell de fons el model ΛCDM estàndard, els components foscos evolucionen de manera molt diferent. Per estudiar-los rigorosament, els codis numèrics de les pertorbacions cosmològiques han de ser adequadament modificats, amb l'inconvenient d'incrementar notablement el temps de càlcul. Aquest fet és alleujat al § 9, on un nou mètode per calcular l'espectre de potència dels models d'energia fosca és proposat. Finalment, en el § 10 tres noves parametritzacions del paràmetre de desacceleració, amb base a arguments termodinàmics sòlids, es proposen i es contrasta amb les dades observacionals.Nowadays the Universe appears to be undergoing a phase of accelerated expansion, as witnessed by supernovae data and later corroborated by a host a cosmological measurements -very recently by the Planck satellite. While this expansion can be described in Einstein’s theory of gravity by invoking the existence of a positive but exceedingly small cosmological constant, Λ, connected to the quantum vacuum, many alternative, and sometimes sophisticated, explanations have been proposed. Roughly, the energy content of the present universe can be split into 5% of baryonic matter and 95% of a non-visible (dubbed the “dark sector” because its components do not interact electromagnetically) whose 25% consists of non-relativistic, weakly interacting massive particles (“cold dark matter”) and a 75% of a component with a huge negative pressure, the so-called “dark energy”. The nature of the latter component is completely unknown; this justifies that many “trial” candidates have been proposed. By far, the simplest and most successful one is the cosmological constant, mentioned above. However, it suffers from two main drawbacks at the theoretical level: the coincidence problem and the fine tuning problem. The aim of this Memoir is to propose and constrain cosmological models of dark energy that circumvent these difficulties. This Memoir is organized as follows: The Chapters §2, §3 and §4 introduce basic concepts widely used when considering the different models that conforms our research work. The following Chapters focus on the different cosmological models. In §5 dark energy is considered connected to the holographic principle and posits that it interacts (also non-gravitationally) with dark matter. The holographic principle sets a length scale, in this case the Hubble length, i.e., the scale of the causally connected events. In §6 the previous model is studied more deeply and an alternative to it is presented. Both models share identical background evolution but each component behaves differently, which induces a diverse behavior at the perturbative level. This allows to observationally discriminate one model from the other. A further holographic dark energy model is proposed in §7; this one based on the Ricci length (i.e., the maximum size a perturbation can have leading to a black hole). Again, a non-gravitational interaction is assumed between dark energy and dark matter. In §8, a unified dark model (featuring a unification between dark matter ad dark energy) previously proposed is studied. Since the parameter space that fits the observational data is very narrow (and also in view of its theoretical interest), we decompose the single energy component into cold dark matter and quantum vacuum interacting with one another. As a consequence the allowed parameter space gets substantially augmented. Although the models mentioned above mimic at the background level the standard ΛCDM model, the dark components evolve very differently. To rigorously study them, the numerical codes for the cosmological perturbations must be suitably modified, with the drawback of notably increasing the computational time. This is much alleviated in §9 where a novel method to calculate the matter power spectrum of dark energy models is proposed. Finally, in §10 three model independent parameterizations of the deceleration parameter, based on solid thermodynamic arguments, are proposed and contrasted with the observational data.
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Tamanini, N. "Dynamical systems in dark energy models." Thesis, University College London (University of London), 2014. http://discovery.ucl.ac.uk/1456304/.
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This PhD thesis is devoted to the study of dynamical systems appearing in theoretical models of dark energy. The quest for understanding the origin of the observed cosmic acceleration has led physicists to advance a large number of phenomenological explanations based on different fundamental theories. The best approach to analyse the background cosmological impli- cations of all these models consists in employing dynamical systems tech- niques. In this thesis, after reviewing elements of dynamical systems theory and basic cosmology, several dynamical systems, which arise in dark energy models ranging from scalar fields to modified gravity, will be studied using both analytical and numerical methods. The work is organised in order to present as many details as possible for the simpler and well known models, while outlining major results and referring to the literature for the less stud- ied ones. This choice aims at providing the reader with a complete overview and summary of dynamical systems in dark energy applications.
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Costa, André Alencar da. "Observational Constraints on Models with an Interaction between Dark Energy and Dark Matter." Universidade de São Paulo, 2014. http://www.teses.usp.br/teses/disponiveis/43/43134/tde-20012015-123002/.
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In this thesis we go beyond the standard cosmological LCDM model and study the effect of an interaction between dark matter and dark energy. Although the LCDM model provides good agreement with observations, it faces severe challenges from a theoretical point of view. In order to solve such problems, we first consider an alternative model where both dark matter and dark energy are described by fluids with a phenomenological interaction given by a combination of their energy densities. In addition to this model, we propose a more realistic one based on a Lagrangian density with a Yukawa-type interaction. To constrain the cosmological parameters we use recent cosmological data, the CMB measurements made by the Planck satellite, as well as BAO, SNIa, H0 and Lookback time measurements.Nesta tese vamos além do modelo cosmológico padrão, o LCDM, e estudamos o efeito de uma interação entre a matéria e a energia escuras. Embora o modelo LCDM esteja de acordo com as observações, ele sofre sérios problemas teóricos. Com o objetivo de resolver tais problemas, nós primeiro consideramos um modelo alternativo, onde ambas, a matéria e a energia escuras, são descritas por fluidos com uma interação fenomenológica dada como uma combinação das densidades de energia. Além desse modelo, propomos um modelo mais realista baseado em uma densidade Lagrangiana com uma interação tipo Yukawa. Para vincular os parâmetros cosmológicos usamos dados cosmológicos recentes como as medidas da CMB feitas pelo satélite Planck, bem como medidas de BAO, SNIa, H0 e Lookback time.
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Zsembinszki, Gabriel. "Light scalar fields in a dark universe: models of inflation, dark energy and dark matter." Doctoral thesis, Universitat Autònoma de Barcelona, 2007. http://hdl.handle.net/10803/3390.
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La teoría científica de más éxito hoy en día, sobre el origen y la evolución del universo, es conocida como el modelo estándar del Big Bang, el cual es una de las construcciones intelectuales más ambiciosas de la humanidad. Se basa en dos ramas bien consolidadas de la física teórica, a saber, la teoría de la Relatividad General y el Modelo Estándar de la física de partículas, y es capaz de hacer predicciones sólidas, como la expansión del universo, la existencia del fondo de radiación de microondas y las abundancias relativas de los elementos ligeros. Algunas de las predicciones teóricas ya han sido confirmadas por observaciones muy precisas.Según la cosmología estándar del Big Bang, el universo primitivo consistía en un plasma muy caliente y denso que se expandió y se enfrió continuamente hasta el presente, dando paso a una serie de transiciones de fase cosmológicas, donde las teorías que describen el universo en cada fase son distintas. Dado que las energías del universo primitivo fueron mucho más altas que las alcanzadas en experimentos terrestres, el estudio del universo primitivo podría ofrecernos importantes informaciones sobre nuevas interacciones y nuevas partículas, abriendo nuevas direcciones para la extensión del Modelo Estándar de la física de partículas.
Como ya he mencionado anteriormente, durante la expansión del universo ocurrieron varias transiciones de fase que dejaron su huella sobre el estado presente del universo. Las observaciones sugieren que durante una de estas transiciones de fase, el universo primitivo sufrió un periodo de expansión acelerada, conocido como inflación. Aunque no forma parte de la cosmología estándar, la inflación es capaz de solucionar de una manera simple y elegante casi todos los problemas relacionados con el modelo estándar del Big Bang, y debería tenerse en cuenta en cualquier extensión posible de la teoría. Las observaciones también revelan la existencia de dos formas de energía desconocidas, a saber, materia oscura y energía oscura. La materia oscura es una forma de materia no relativista y no bariónica, que solamente puede ser detectada indirectamente, mediante su interacción con la materia normal. La energía oscura es un tipo de sustancia con presión negativa, que empezó a dominar recientemente y que es la causa de la aceleración de la expansión del universo.
En esta tesis doctoral presento varios modelos originales propuestos para resolver algunos de los problemas de la cosmología estándar, como posibles extensiones del modelo del Big Bang. Algunos de estos modelos introducen nuevas simetrías y partículas con el fin de explicar la inflación y la energía oscura y/o la materia oscura en una descripción unificada. Uno de los modelos es propuesto para explicar la energía oscura del universo, a través de un nuevo campo escalar que oscila en un potencial.
The most successful scientific theory today about the origin and evolution of the universe is known as the standard Big Bang model, which is one of the most ambitious intellectual constructions of the humanity. It is based on two consolidated branches of theoretical physics, namely, the theory of General Relativity and the Standard Model of particle physics, and is able to make robust predictions, such as the expansion of the universe, the existence of the cosmic microwave background radiation and the relative primordial abundance of light elements. Some of the theoretical predictions have already been confirmed by very precise observations.
According to the standard Big Bang cosmology, the early universe consisted of a very hot and dense plasma that continuously expanded and cooled up to the present, giving place to a series of cosmological phase transitions, where the theories describing the universe in each phase are different. Given that the energies of the early universe were much higher than those reached in terrestrial experiments, the study of the early universe might give us important information about new interactions and new particles, opening new directions for extending the Standard Model of particle physics.
As already mentioned above, during the expansion of the universe, different phase transitions occurred, which left their imprint on the present state of the universe. Observations suggest that during a very early phase transition the universe suffered a stage of accelerated expansion, known as inflation. Although inflation is not included in the standard cosmology, it is able to solve in a simple and elegant manner almost all of the shortcomings related to the standard Big Bang model, and should be taken into account in any possible extension of the theory. Observations also reveal evidence of the existence of two unknown forms of energy, i.e., dark matter and dark energy. Dark matter is a form of non-relativistic and non-baryonic matter, which can only be detected indirectly, by its gravitational interactions with normal matter. Dark energy is a kind of substance with negative pressure, which started to dominate recently and causes the accelerated expansion of the universe.
In this PhD Thesis, I present a few original models proposed to solve some of the shortcomings of the standard cosmology, as possible extensions of the Big Bang model. Some of these models introduce new symmetries and particles in order to explain inflation and dark energy and/or dark matter in a unified description. One of the models is proposed for explaining the dark energy of the universe, by means of a new scalar field oscillating in a potential.
The most successful scientific theory today about the origin and evolution of the universe is known as the standard Big Bang model, which is one of the most ambitious intellectual constructions of the humanity. It is based on two consolidated branches of theoretical physics, namely, the theory of General Relativity and the Standard Model of particle physics, and is able to make robust predictions, such as the expansion of the universe, the existence of the cosmic microwave background radiation and the relative primordial abundance of light elements. Some of the theoretical predictions have already been confirmed by very precise observations.
According to the standard Big Bang cosmology, the early universe consisted of a very hot and dense plasma that continuously expanded and cooled up to the present, giving place to a series of cosmological phase transitions, where the theories describing the universe in each phase are different. Given that the energies of the early universe were much higher than those reached in terrestrial experiments, the study of the early universe might give us important information about new interactions and new particles, opening new directions for extending the Standard Model of particle physics.
As already mentioned above, during the expansion of the universe, different phase transitions occurred, which left their imprint on the present state of the universe. Observations suggest that during a very early phase transition the universe suffered a stage of accelerated expansion, known as inflation. Although inflation is not included in the standard cosmology, it is able to solve in a simple and elegant manner almost all of the shortcomings related to the standard Big Bang model, and should be taken into account in any possible extension of the theory. Observations also reveal evidence of the existence of two unknown forms of energy, i.e., dark matter and dark energy. Dark matter is a form of non-relativistic and non-baryonic matter, which can only be detected indirectly, by its gravitational interactions with normal matter. Dark energy is a kind of substance with negative pressure, which started to dominate recently and causes the accelerated expansion of the universe.
In this PhD Thesis, I present a few original models proposed to solve some of the shortcomings of the standard cosmology, as possible extensions of the Big Bang model. Some of these models introduce new symmetries and particles in order to explain inflation and dark energy and/or dark matter in a unified description. One of the models is proposed for explaining the dark energy of the universe, by means of a new scalar field oscillating in a potential.
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Mania, Data. "Constraints on dark energy models from observational data." Thesis, Kansas State University, 2012. http://hdl.handle.net/2097/14178.
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Master of ScienceDepartment of Physics
Bharat Ratra
Recent observations in cosmology suggest that the universe is undergoing accelerating expansion. Mysterious component responsible for acceleration is called "Dark Energy" contributing to 70% of total energy density of the universe. Simplest DE model is [Lambda]CDM, where Einstein’s cosmological constant plays role of the dark energy. Despite the fact that it is consistent with observational data, it leaves some important theoretical questions unanswered. To overcome these difficulties different Dark energy models are proposed. Two of these models XCDM parametrization and slow rolling scalar field model [phi]CDM, along with "standard" [Lambda]CDM are disscussed here, constraining their parameter set. In this thesis we start with a general theoretical overview of basic ideas and distance measures in cosmology. In the following chapters we use H II starburst galaxy apparent magnitude versus redshift data from Siegel et al.(2005) to constrain DE model parameters. These constraints are generally consistent with those derived using other data sets, but are not as restrictive as the tightest currently available constraints. Also we constrain above mentioned cosmological models in light of 32 age measurements of passively evolving galaxies as a function of redshift and recent estimates of the product of the cosmic microwave background acoustic scale and the baryon acoustic oscillation peak scale.
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Rivera, Echeverri José David [UNESP]. "ISW effect through dark energy quintessence and ΛCDM models." Universidade Estadual Paulista (UNESP), 2013. http://hdl.handle.net/11449/92030.
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Observações atuais do satélite Wilkinson Microwave Anisotropy Probe (WMAP) da Radiação Cósmica de Fundo (CMB) e estruturas de grande escala (LSS) têm permitido melhorar os estudos das anisotropias secundárias, especialmente o efeito Sachs-Wolfe Integrado (ISW). Usando a correlação cruzada entre a CMB e mapas da LSS, o sinal do efeito ISW pode ser detectado. Nós podemos usar o efeito ISW junto com o modelo cosmológico padrão (neste caso o Universo esta dominado pela constante cosmológica e a Matéria Escura Fria, ΛCDM) mais algoritmos numéricos para restringir os parâmetros em um modelo cosmológico com energia escura. Para diferentes casos com um único parâmetro livre de um model de Quintessência parametrizado,' w IND. 0' < 0 e 2,0 < 'w IND. a' <−2,0, podemos encontrar bins de largura [−1,926,−0,323] em 'w ind. 0' e [−0,855, 1,190]. Nestes intervalos, obtemos um sigma de nivel tomando o 68% da amostra que melhor se ajusta ao modelo cosmológico padrão
Current observations of the Wilkinson Microwave Anisotropy Probe (WMAP) satellite of Cosmic Microwave Background (CMB) and Large Scale Structure (LSS) have allowed to improve studies of the secondary anisotropies, especially the Integrated Sachs-Wolfe effect (ISW). Using the cross-correlation between the CMB and LSS maps, the ISW effect signal can be detected. We can use the ISW effect together with standard cosmological model (in this case the Universe is dominated by the cosmological constant and Cold Dark Matter, ΛCDM) plus numerical algorithms to constrain the parameters in a cosmological model with dark energy. For cases different with a single free parameter of a parameterised Quintessence model, 'w ind. 0' < 0 and 2,0 < 'w ind. a' <−2,0, we can find bins of width [−1,926,−0,323] in 'w ind. 0' and [−0,855, 1,190] in wa. In these intervals, we obtain one sigma level by taking the 68% of the sample which best fit the standard cosmological model
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Rivera, Echeverri José David. "ISW effect through dark energy quintessence and ΛCDM models /." São Paulo, 2013. http://hdl.handle.net/11449/92030.
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Orientador: Maria Cristina Batoni Abdalla RibeiroCoorientador: Felipe Batoni Abdalla
Banca: Marcos Vinícius Borges Teixeira Lima
Banca: Laerte Sodré Junior
Resumo: Observações atuais do satélite Wilkinson Microwave Anisotropy Probe (WMAP) da Radiação Cósmica de Fundo (CMB) e estruturas de grande escala (LSS) têm permitido melhorar os estudos das anisotropias secundárias, especialmente o efeito Sachs-Wolfe Integrado (ISW). Usando a correlação cruzada entre a CMB e mapas da LSS, o sinal do efeito ISW pode ser detectado. Nós podemos usar o efeito ISW junto com o modelo cosmológico padrão (neste caso o Universo esta dominado pela constante cosmológica e a Matéria Escura Fria, ΛCDM) mais algoritmos numéricos para restringir os parâmetros em um modelo cosmológico com energia escura. Para diferentes casos com um único parâmetro livre de um model de Quintessência parametrizado,' w IND. 0' < 0 e 2,0 < 'w IND. a' <−2,0, podemos encontrar bins de largura [−1,926,−0,323] em 'w ind. 0' e [−0,855, 1,190]. Nestes intervalos, obtemos um sigma de nivel tomando o 68% da amostra que melhor se ajusta ao modelo cosmológico padrão
Abstract: Current observations of the Wilkinson Microwave Anisotropy Probe (WMAP) satellite of Cosmic Microwave Background (CMB) and Large Scale Structure (LSS) have allowed to improve studies of the secondary anisotropies, especially the Integrated Sachs-Wolfe effect (ISW). Using the cross-correlation between the CMB and LSS maps, the ISW effect signal can be detected. We can use the ISW effect together with standard cosmological model (in this case the Universe is dominated by the cosmological constant and Cold Dark Matter, ΛCDM) plus numerical algorithms to constrain the parameters in a cosmological model with dark energy. For cases different with a single free parameter of a parameterised Quintessence model, 'w ind. 0' < 0 and 2,0 < 'w ind. a' <−2,0, we can find bins of width [−1,926,−0,323] in 'w ind. 0' and [−0,855, 1,190] in wa. In these intervals, we obtain one sigma level by taking the 68% of the sample which best fit the standard cosmological model
Mestre
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Pavlov, Anatoly. "Constraining competing models of dark energy with cosmological observations." Diss., Kansas State University, 2015. http://hdl.handle.net/2097/20345.
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Doctor of PhilosophyDepartment of Physics
Bharat Ratra
The last decade of the 20th century was marked by the discovery of the accelerated expansion of the universe. This discovery puzzles physicists and has yet to be fully understood. It contradicts the conventional theory of gravity, i.e. Einstein’s General Relativity (GR). According to GR, a universe filled with dark matter and ordinary matter, i.e. baryons, leptons, and photons, can only expand with deceleration. Two approaches have been developed to study this phenomenon. One attempt is to assume that GR might not be the correct description of gravity, hence a modified theory of gravity has to be developed to account for the observed acceleration of the universe’s expansion. This approach is known as the ”Modified Gravity Theory”. The other way is to assume that the energy budget of the universe has one more component which causes expansion of space with acceleration on large scales. Dark Energy (DE) was introduced as a hypothetical type of energy homogeneously filling the entire universe and very weakly or not at all interacting with ordinary and dark matter. Observational data suggest that if DE is assumed then its contribution to the energy budget of the universe at the current epoch should be about 70% of the total energy density of the universe. In the standard cosmological model a DE term is introduced into the Einstein GR equations through the cosmological constant, a constant in time and space, and proportional to the metric tensor g[subscript]mu[subscript]nu. While this model so far fits most available observational data, it has some significant conceptual shortcomings. Hence there are a number of alternative cosmological models of DE in which the dark energy density is allowed to vary in time and space.
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Weller, Joel Martin. "Models of onflation and dark energy with coupled scalar fields." Thesis, University of Sheffield, 2011. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.538088.
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Saha, Arindam. "Modified theories of gravity and dark energy models of the universe." Thesis, University of North Bengal, 2013. http://hdl.handle.net/123456789/964.
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Braglia, Matteo. "Initial conditions for cosmological perturbations in scalar-tensor dark-energy models." Master's thesis, Alma Mater Studiorum - Università di Bologna, 2017. http://amslaurea.unibo.it/13860/.
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We discuss the evolution and imprints of isocurvature initial conditions for the scalar field in scalar tensor extensions of Einstein gravity. We consider the simplest models of scalar tensor theories, as Induced gravity (IG, which can be recasted in form of Jordan-Brans-Dicke theory by a redefinition of the scalar field) or non-minimally coupled (NMC) scalar fields in which the acceleration of the Universe is connected to a variation of the effective Planck mass. After introducing the fundamental ideas of cosmological perturbation theory and scalar tensor theories of gravity, we give the evolution equations for matter, metric and scalar field fluctuations in synchronous gauge. We use this set of equations for both the IG and the NMC models to find a new isocurvature solution in which the scalar field fluctuations compensate for the relativistic components respectively. We also show how we can generalize the well known isocurvature modes in Einstein GR to these models. We show the different evolution of cosmological fluctuations for these isocurvature initial conditions compared to the standard adiabatic one. After that, we compute the CMB angular power spectrum for these solutions in the IG model, with the help of a modified Einstein-Boltzmann CLASS code. In particular the CMB power spectrum is computed separately for adiabatic and isocurvature initial conditions, i.e. for totally uncorrelated modes, and with arbitrary correlations leading to an interesting explanation of the lack of power in the low multipoles region of the CMB temperature power spectrum. Finally we show how a simple model of double inflation in IG could explain the generation of the new isocurvature mode.
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Marcondes, Rafael José França. "Interacting dark energy models in Cosmology and large-scale structure observational tests." Universidade de São Paulo, 2016. http://www.teses.usp.br/teses/disponiveis/43/43134/tde-17102016-123725/.
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Modern Cosmology offers us a great understanding of the universe with striking precision, made possible by the modern technologies of the newest generations of telescopes. The standard cosmological model, however, is not absent of theoretical problems and open questions. One possibility that has been put forward is the existence of a coupling between dark sectors. The idea of an interaction between the dark components could help physicists understand why we live in an epoch of the universe where dark matter and dark energy are comparable in terms of energy density, which can be regarded as a strange coincidence given that their time evolutions are completely different. Dark matter and dark energy are generally treated as perfect fluids. Interaction is introduced when we allow for a non-zero term in the right-hand side of their individual energy-momentum tensor conservation equations. We proceed with a phenomenological approach to test models of interaction with observations of redshift-space distortions. In a flat universe composed only of these two fluids, we consider separately two forms of interaction, through terms proportional to the densities of both dark energy and dark matter. An analytic expression for the growth rate approximated as f = Omega^gamma, where Omega is the percentage contribution from the dark matter to the energy content of the universe and gamma is the growth index, is derived in terms of the interaction strength and of other parameters of the model in the first case, while for the second model we show that a non-zero interaction cannot be accommodated by the index growth approximation. The successful expressions obtained are then used to compare the predictions with growth of structure observational data in a Markov Chain Monte Carlo code and we find that the current growth data alone cannot impose constraints on the interaction strength due to their large uncertainties. We also employ observations of galaxy clusters to assess their virial state via the modified Layzer-Irvine equation in order to detect signs of an interaction. We obtain measurements of observed virial ratios, interaction strength, rest virial ratio and departure from equilibrium for a set of clusters. A compounded analysis indicates an interaction strength of 0.29^{+2.25}_{-0.40}, compatible with no interaction, but a compounded rest virial ratio of 0.82^{+0.13}_{-0.14}, which means a 2 sigma confidence level detection. Despite this tension, the method produces encouraging results while still leaves room for improvement, possibly by removing the assumption of small departure from equilibrium.A cosmologia moderna oferece um ótimo entendimento do universo com uma precisão impressionante, possibilitada pelas tecnologias modernas das gerações mais novas de telescópios. O modelo cosmológico padrão, porém, não é livre de problemas do ponto de vista teórico, deixando perguntas ainda sem respostas. Uma possibilidade que tem sido proposta é a existência de um acoplamento entre setores escuros. A ideia de uma interação entre os componentes escuros poderia ajudar os físicos a entender por que vivemos em uma época do universo na qual a matéria escura e a energia escura são comparáveis em termos de densidades de energia, o que pode ser considerado uma estranha coincidência dado que suas evoluções com o tempo são completamente diferentes. Matéria escura e energia escura são geralmente tratadas como fluidos perfeitos. A interação é introduzida ao permitirmos um tensor não nulo no lado direito das equações de conservação dos tensores de energia-momento. Prosseguimos com uma abordagem fenomenológica para testar modelos de interação com observações de distorções no espaço de redshift. Em um universo plano composto apenas por esses dois fluidos, consideramos, separadamente, duas formas de interação, através de termos proporcionais às densidades de energia escura e de matéria escura. Uma expressão analítica para a taxa de crescimento aproximada por f = Omega^gamma, onde Omega é a contribuição percentual da matéria escura para o conteúdo do universo e gamma é o índice de crescimento, é deduzida em termos da interação e de outros parâmetros do modelo no primeiro caso, enquanto para o segundo caso mostramos que uma interação não nula não pode ser acomodada pela aproximação do índice de crescimento. As expressões obtidas são então utilizadas para comparar as previsões com dados observacionais de crescimento de estruturas em um programa para Monte Carlo via cadeias de Markov. Concluímos que tais dados atuais por si só não são capazes de restringir a interação devido às suas grandes incertezas. Utilizamos também observações de aglomerados de galáxias para analisar seus estados viriais através da equação de Layzer-Irvine modificada a fim de detectar sinais de interação. Obtemos medições de taxas viriais observadas, constante de interação, taxa virial de equilíbrio e desvio do equilíbrio para um conjunto de aglomerados. Uma análise combinada indica uma constante de interação 0.29^{+2.25}_{-0.40}, compatível com zero, mas uma taxa virial de equilíbrio combinada de 0.82^{+0.13}_{-0.14}, o que significa uma detecção em um intervalo de confiança de 2 sigma. Apesar desta tensão, o método produz resultados encorajadores enquanto ainda permite melhorias, possivelmente pela remoção da suposição de pequenos desvios do equilíbrio.
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Shojaei, Hamed. "Interacting dark energy models as an approach for solving Cosmic Coincidence Problem." [Bloomington, Ind.] : Indiana University, 2009. http://gateway.proquest.com/openurl?url_ver=Z39.88-2004&rft_val_fmt=info:ofi/fmt:kev:mtx:dissertation&res_dat=xri:pqdiss&rft_dat=xri:pqdiss:3378380.
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Thesis (Ph.D.)--Indiana University, Dept. of Physics, 2009.Title from PDF t.p. (viewed on Jul 12, 2010). Source: Dissertation Abstracts International, Volume: 70-10, Section: B, page: 6316. Adviser: Mike Berger.
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Caldera-Cabral, Gabriela A. "Interacting dark energy models of the late-time acceleration of the Universe." Thesis, University of Portsmouth, 2009. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.507159.
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D'Angelo, Beatrice. "Density and velocity profiles in dark scattering models." Master's thesis, Alma Mater Studiorum - Università di Bologna, 2018. http://amslaurea.unibo.it/16210/.
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Per quanto la cosmologia osservativa odierna sia in una fase di precisione senza precedenti, con i dati CMB, BAO, e Supernovae Ia che mostrano di essere in accordo con l’attuale modello LCDM, i dati Planck sono in tensione con quelli a basso redshift, provenienti ad esempio dal misurazioni di weak lensing, che puntano verso un tasso più basso di crescita delle strutture.
I modelli Dark Scattering qui trattati sono caratterizzati dalla evoluzione di un campo scalare classico con il ruolo di DE, e dalla interazione che le particelle di Materia Oscura (DM) hanno con questo campo. Considerando le particelle DM in moto attraverso il fluido DE, esse osservano un flusso di momento diverso da zero, indice di una forza proporzionale alla sezione d'urto di scattering tra DE e DM.
Nel presente lavoro sono stati analizzati dati provenienti da simulazioni cosmologiche N-body DM-only per cinque modelli: due a equazione di stato DE costante, due con equazione di stato dipendente dal tempo, e infine il modello standard LCDM come base di confronto. Le condizioni iniziali sono uguali per tutti i modelli, in modo tale che ogni differenza rilevata nei risultati sia riconducibile agli effetti dei diversi modelli cosmologici.
Sono stati ricavati i profili di densità e, per la prima volta su questi dati, i profili di velocità, di un significativo di aloni di materia oscura per ogni cosmologia, divisi in bin di massa e per tre redshift.
Viene evidenziato come il termine aggiuntivo di drag nei modelli dark scattering abbia due effetti diversi nella crescita delle strutture. Nel regime lineare, infatti, le particelle DM in infall verso il centro degli ammassi hanno una direzione radiale del moto e l'attrito con il fluido DE le fa rallentare, diminuendo la loro velocità. Quando passano al regime non lineare, acquistano una componente tangenziale di velocità che di fatto fa sì che l'interazione con l'energia oscura provochi una perdita di energia cinetica con conseguente collasso più rapido.
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Martineau, Patrick. "Topics in cosmological fluctuations : linear order and beyond." Thesis, McGill University, 2007. http://digitool.Library.McGill.CA:80/R/?func=dbin-jump-full&object_id=111877.
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The object of this thesis is to present various applications of the theory of cosmological perturbations. Within are contained a number of manuscripts, each concerned with a separate aspect of the theory. The thesis itself begins with a general overview of cosmological perturbation theory designed to be accessible to the non-specialist. Both the classical and quantum first order theory are considered. Back-reaction, via the formalism of the Effective Energy Momentum Tensor (EEMT) is reviewed. Subsequent chapters are more specialized dealing with various applications of the theory. At first order, topics discussed include the classicalization of cosmological perturbations (chapter 2), and the effects of including the dilaton and its fluctuations on a novel mechanism for the production of inhomogeneities in string gas cosmology (chapter 3). At second order, an original solution to the Dark Energy problem is proposed (chapter 4), and the effects of back-reaction on the power spectrum, including the spectral index and the gaussianity, are examined (chapter 5).
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Redzikultsava, Katazhyna. "Testing the limits of alternative cosmologies and chasing the dream data set." Thesis, The University of Sydney, 2019. https://hdl.handle.net/2123/21330.
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The universe is accelerating, yet we know very little about the mysterious energy making it behave this way. Scientists put forward model after model, proposing arrays of cosmological fluids capable of causing acceleration. These models are fitted to data, and results are compared against each other. But how good is the current data at telling models apart? And what makes a better data set? The first aim of this thesis is to investigate what else might be hiding in the existing supernova data. This is done by generating and fitting increasingly strange, parameter-rich cosmological models. The second aim is to define such boundaries for the supernova data (sample size and uncertainty) which, if met, will allow scientists to rule out some of the more extreme contenders. This thesis explores the limits of the current supernova data, as well as its future potential. For the first part I found that, as far as the currently available data is concerned, our underlying cosmology may be very wild indeed. And as for the perfect data set? That remains to be seen.
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Ghose, Souvik. "SOME ASPECTS OF MODIFIED THEORIES OF GRAVITY AND DARK ENERGY MODELS OF THE UNIVERSE." Thesis, University of North Bengal, 2013. http://hdl.handle.net/123456789/967.
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Barello, Gregory. "Models and Constraints for New Physics at the Energy, Intensity, and Cosmic Frontiers." Thesis, University of Oregon, 2016. http://hdl.handle.net/1794/20454.
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The modern era of particle physics is driven by experimental anomalies. Experimental efforts have become increasingly diverse and are producing enormous volumes of data. In such a highly data-driven scientific environment theoretical models are necessary to understand this data and to help inform the development of new experimental approaches. In this dissertation I present two significant contributions to this effort relevant to the energy, intensity, and cosmic frontiers of modern particle physics research.
Part 1 of this dissertation discusses methods to understand modern dark matter direct detection results. In particular I present an analysis under the hypothesis of inelastic dark matter, which supposes that dark matter must scatter inelastically, i.e. that it must gain or loose mass during a collision with atomic nuclei. This hypothesis is attractive because it can alleviate otherwise contradictory results from a number of dark matter detection facilities. The main conclusion of this work is a presentation of the analytical tools, along with a mathematica package that can be used to run the analysis, and the discovery that there are regions of inelastic dark matter parameter space which are consistent with all current experimental results, and constraints.
Part 2 of this dissertation discusses a phenomenon of modern interest called kinetic mixing which allows particles from the standard model to spontaneously transform into particles which experience a new, as of yet undiscovered, force. This phenomenon is relatively common and well motivated theoretically and has motivated significant experimental effort. In this work, I present an analysis of a general case of kinetic mixing, called nonabelian kinetic mixing. This work shows that, In general, kinetic mixing predicts the existence of a new particle and that, under certain conditions, this particle could be detected at modern particle colliders. Furthermore, the mass of this particle is related to the strength of kinetic mixing. This relationship suggests novel ways to constrain kinetic mixing parameter space, and if observed would provide a very striking indication that such a model is realized in nature.
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Garaldi, Enrico. "Zoomed simulations of Halo segregation in cosmological models with two species of coupled dark matter." Master's thesis, Alma Mater Studiorum - Università di Bologna, 2014. http://amslaurea.unibo.it/7592/.
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La materia ordinaria copre soli pochi punti percentuali della massa-energia totale dell'Universo, che è invece largamente dominata da componenti “oscure”. Il modello standard usato per descriverle è il modello LambdaCDM. Nonostante esso sembri consistente con la maggior parte dei dati attualmente disponibili, presenta alcuni problemi fondamentali che ad oggi restano irrisolti, lasciando spazio per lo studio di modelli cosmologici alternativi.
Questa Tesi mira a studiare un modello proposto recentemente, chiamato “Multi-coupled Dark Energy” (McDE), che presenta interazioni modificate rispetto al modello LambdaCDM. In particolare, la Materia Oscura è composta da due diversi tipi di particelle con accoppiamento opposto rispetto ad un campo scalare responsabile dell'Energia Oscura. L'evoluzione del background e delle perturbazioni lineari risultano essere indistinguibili da quelle del modello LambdaCDM.
In questa Tesi viene presentata per la prima volta una serie di simulazioni numeriche “zoomed”. Esse presentano diverse regioni con risoluzione differente, centrate su un singolo ammasso di interesse, che permettono di studiare in dettaglio una singola struttura senza aumentare eccessivamente il tempo di calcolo necessario.
Un codice chiamato ZInCo, da me appositamente sviluppato per questa Tesi, viene anch'esso presentato per la prima volta. Il codice produce condizioni iniziali adatte a simulazioni cosmologiche, con differenti regioni di risoluzione, indipendenti dal modello cosmologico scelto e che preservano tutte le caratteristiche dello spettro di potenza imposto su di esse.
Il codice ZInCo è stato usato per produrre condizioni iniziali per una serie di simulazioni numeriche del modello McDE, le quali per la prima volta mostrano, grazie all'alta risoluzione raggiunta, che l'effetto di segregazione degli ammassi avviene significativamente prima di quanto stimato in precedenza. Inoltre, i profili radiale di densità ottenuti mostrano un appiattimento centrale nelle fasi iniziali della segregazione. Quest'ultimo effetto potrebbe aiutare a risolvere il problema “cusp-core” del modello LambdaCDM e porre limiti ai valori dell'accoppiamento possibili.
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Williams, Jolin Shan. "Dynamics of Discrete Irregular Cosmological Models." Thesis, Stockholms universitet, Fysikum, 2014. http://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-110841.
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This thesis investigates the dynamics of a set of 8-600 Schwarzschild masses, randomly distributed inside cells which tessellate a 3-sphere. Furthermore the contents of each cell are mirror images of its neighbor. This symmetry give rise to a locally rotationally symmetric (LRS) curve, along which the Einstein field equations governing dynamics can be exactly integrated. The result is an irregular model consisting of discrete matter content, but where the dynamics is easy to calculate. We see that these local inhomogeneities will cause behavior deviating from the spherical dust-filled FLRW model. For instance, there are cases where configurations exhibit acceleration along the LRS curve, even though the content consists solely of ordinary matter with a vacuum filled exterior and no cosmological constant.Denna avhandling undersöker konfigurationer av 8-600 Schwarzschild-massor, som är slumpmässigt utplacerade inom celler som tessellerar en 3-sfär. Utöver det är även innehållet i varje cell en spegelbild av granncellen. Denna symmetri ger upphov till en lokalt rotationssymmetrisk (LRS) kurva där Einsteins fältekvationer som beskriver dynamiken längs med är exakt integrerbara. Resultatet är en oregelbunden modell som består av diskreta massor, men vars dynamik är enkel att beräkna. Vi ser att dessa lokala inhomogeniteter ger upphov till beteenden som avviker från den sfäriska partikel-fyllda FLRW-modellen. Till exempel uppstår konfigurationer som uppvisar acceleration längs med LRS-kurvan, trots att innehållet består endast av ordinära massor med vakuum utanför och ingen kosmologisk konstant.
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Ballardini, Mario <1986>. "Cosmological Constraints on Cosmic Inflation and Scalar-Tensor Dark Energy Models from CMB Anisotropies and Galaxy Clustering." Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2016. http://amsdottorato.unibo.it/7764/1/Thesis.pdf.
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This thesis investigates the most recent cosmological bservations in order to constrain cosmic inflation and what is probably the simplest model of modified gravity.
We provide a detailed calculation for the scalar spectral index and for the tensor-to-scalar ratio, in slow-roll approximation, for a selection of single field inflationary models and we compare them with Planck 2015 data, taking into account reheating uncertainties.
We studied selected theoretically motivated parametrizations of the primordial power spectrum with departure from the near scale invariance, providing a better
fit to the CMB temperature power spectrum with respect to the simplest slow-roll inflationary models. For a selection of models, we forecast the capability of future spectroscopic, photometric, and radio surveys, in combination with CMB measurements, to constrain parametrized features in the primordial power spectrum.
We studied a simple class of modified gravity models alternative to ΛCDM, based on Induced Gravity, or a Brans-Dicke like, with a monomial potential with positive
values of the exponent. Cosmological constraints for this class of dark energy models are derived from CMB alone and in combination with external dataset, such as BAO
and H0 local measurements.
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Casas, Castro Santiago [Verfasser], and Valeria [Akademischer Betreuer] Pettorino. "Non-linear structure formation in models of Dark Energy and Modified Gravity / Santiago Casas Castro ; Betreuer: Valeria Pettorino." Heidelberg : Universitätsbibliothek Heidelberg, 2017. http://d-nb.info/118098630X/34.
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Casas, Santiago [Verfasser], and Valeria [Akademischer Betreuer] Pettorino. "Non-linear structure formation in models of Dark Energy and Modified Gravity / Santiago Casas Castro ; Betreuer: Valeria Pettorino." Heidelberg : Universitätsbibliothek Heidelberg, 2017. http://d-nb.info/118098630X/34.
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Feix, Martin. "Extragalactic and cosmological tests of gravity theories with additional scalar or vector fields." Thesis, University of St Andrews, 2011. http://hdl.handle.net/10023/1901.
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Despite the many successes of the current standard model of cosmology on the largest physical scales, it relies on two phenomenologically motivated constituents, cold dark matter and dark energy, which account for approximately 95% of the energy-matter content of the universe. From a more fundamental point of view, however, the introduction of a dark energy (DE) component is theoretically challenging and extremely fine-tuned, despite the many proposals for its dynamics. On the other hand, the concept of cold dark matter (CDM) also suffers from several issues such as the lack of direct experimental detection, the question of its cosmological abundance and problems related to the formation of structure on small scales. A perhaps more natural solution might be that the gravitational interaction genuinely differs from that of general relativity, which expresses itself as either one or even both of the above dark components. Here we consider different possibilities on how to constrain hypothetical modifications to the gravitational sector, focusing on the subset of tensor-vector-scalar (TeVeS) theory as an alternative to CDM on galactic scales and a particular class of chameleon models which aim at explaining the coincidences of DE. Developing an analytic model for nonspherical lenses, we begin our analysis with testing TeVeS against observations of multiple-image systems. We then approach the role of low-density objects such as cosmic filaments in this framework and discuss potentially observable signatures. Along these lines, we also consider the possibility of massive neutrinos in TeVeS theory and outline a general approach for constraining this hypothesis with the help of cluster lenses. This approach is then demonstrated using the cluster lens A2390 with its remarkable straight arc. Presenting a general framework to explore the nonlinear clustering of density perturbations in coupled scalar field models, we then consider a particular chameleon model and highlight the possibility of measurable effects on intermediate scales, i.e. those relevant for galaxy clusters. Finally, we discuss the prospects of applying similar methods in the context of TeVeS and present an ansatz which allows to cast the linear perturbation equations into a more convenient form.
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VILAR, NETA Deusalete Câmara. "Defeitos e Modelos de Quintessência." Universidade Federal de Campina Grande, 2016. http://dspace.sti.ufcg.edu.br:8080/jspui/handle/riufcg/2135.
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Capes
Modelos cosmológicos envolvendo campos escalares permitem a descrição de uma fase de expansão cósmica acelerada e, portanto, se apresentam como uma alternativa promissora no estudo da inação cósmica e da energia escura. O elemento chave dessa aceleração é a energia escura ou quintessência. Nosso interesse está em analisar soluções cosmológicas baseadas no formalismo de primeira ordem, aqui em particular, o caso para o espaço-tempo plano, por meio do acoplamento de campos escalares, de uma forma não trivial usando o método de extensão. Os resultados obtidos nos permitem calcular parâmetros cosmológicos analíticos, que ilustramos ao longo do texto através de exemplos resolvidos com situações-modelo de possível interesse. Ainda, discutiremos as ferramentas utilizadas em teoria de campos escalares na descrição de defeitos, tomando com o ponto de partida modelos comum campo escalar, e revisando aspectos básicos de teorias que envolvem três campos escalares. Além disso, utilizando o método BPS (Bogomol'nyi, Prasa de Somerfi eld), mostraremos que as soluções das equações de Eüler-Lagrange podem ser satisfeitas através de soluções de equações de primeira ordem. Após todas essas análises, iremos relacionar a teoria de campo escalar com a equação de campo de Einstein. Através dos procedimentos mencionados, esperamos compreender o processo de expansão do Universo acelerado, utilizando as soluções das equações de Friedmann.
Cosmological models involving scalar eld sallow the description of an accelerated cosmic expansion phase, and thus, they appear as apromising alternative in the study of cosmic in action and dark energy. The key element of this acceleration is the dark energy or quintessence. Our interest is to analyze cosmological solutions based on the fi rst-order formalism. In particular, we investigate the case for at space-time, by coupling scalar fi elds in a nontrivial manner using the extension method. The results obtained allowed us to calculate cosmological analytical parameters which are illustrated along the text. Moreover, we will discuss the tools used in scalar eld theory in the defect description, we took as a starting point models with a scalar eld, and by reviewing the basics of theories that involve three scalar elds. Further more, by using the BPS method (Bogomol'nyi, PrasadandSomer eld), we showed that the solutions of the Euler-Lagrange equations can be derived from the fi rst-order diferential equations. After all these analyzes, we will connect the fi eld theory tools with the Einstein eld equation. We hope to understand the expansion process of the accelerated universe through the previous procedures and by using the solutions of the Friedmann equations.
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Huang, Qizhi. "Topics in 21-cm cosmology : foreground models and their subtraction, map reconstruction for wide field of view interferometers and PAON-4 data analysis." Thesis, Université Paris-Saclay (ComUE), 2019. http://www.theses.fr/2019SACLS373/document.
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Certains aspects de l'extraction du signal cosmologique à 21 cm à partir des observations radio, ainsi que le traitement des données interférométriques pour des observations depuis le sol et depuis l'espace ont été étudiés et sont présentés dans cette thèse. J'ai développé un modèle cohérent et à haute résolution du ciel en radio, qui peut fournir une carte complète et précise du ciel, dans la gamme de fréquence 10 MHz à 2,3 GHz, avec une résolution pouvant atteindre une minute d'arc. Le modèle inclut plusieurs sources de rayonnement diffus, en particulier le synchrotron Galactique, les sources radio brillantes du ciel, ainsi qu'un modèle des sources faibles. J'ai également mis au point une méthode pour extraire le signal 21 cm cosmologique, fortement contaminé par les émissions d'avant-plan et le bruit des récepteurs. La méthode utilise une cascade de deux filtres de Wiener, dans l'espace des fréquences d'abord, et ensuite, dans le domaine angulaire. Le premier filtre exploite les variations lentes des émissions d'avant-plan selon la fréquence, tandis que le second filtre exploite les corrélations angulaires du signal cosmologique pour filtrer le bruit des récepteurs, considéré non corrélé entre deux directions différentes. J'ai développé un nouvel algorithme d'imagerie pour les interféromètres en orbite lunaire. Un tel instrument serait idéal pour cartographier le ciel en dessous de 30 MHz; il ne serait en effet pas soumis aux perturbations ionosphériques et serait protégé des interférences électromagnétiques dues aux émissions terrestres. J'ai montré que l'utilisation de la précession du plan orbital du satellite permet de résoudre le problème de la symétrie miroir. La méthode exploite la relation de projection linéaire entre la carte du ciel et les visibilités mesurées, tant dans l'espace angulaire que dans l'espace des harmoniques sphériques pour reconstruire la carte du ciel. L'algorithme d'imagerie gère la complication due à l'ombre de la Lune se déplaçant avec le temps sur le champ de vue des antennes couvrant tout le ciel. Notons que ces effets ne sont pas pris en charge par les algorithmes d'imagerie existants tels que la W-Projection et la WStacking. Enfin, j'ai effectué une première analyse des données de l'interféromètre de transit PAON-4. J'ai évalué la performance globale du réseau en termes de température de bruit et de la réponse des antennes. J'ai pu étalonner avec succès les visibilités, en déterminant à la fois l'amplitude et la phase des termes de gain complexes, tout en corrigeant les décalages de pointage des antennes de PAON4. J'ai ensuite reconstruit la carte du ciel pour une bande de 10 degrés autour de la déclinaison de la source brillante Cygnus A, à partir du flot de données PAON-4 calibré et nettoyé, en appliquant l'algorithme de décomposition en mode m dans l'espace des harmoniques sphériquesSome aspects of extracting cosmological 21cm signal from radio observations, as well as processing of interferometric data for ground based or space born instruments have been studied and discussed in this dissertation. I have developed a high-resolution self-consistent radio whole sky model, which provides an accurate full sky maps in the frequency range from 10 MHz to 2.3 GHz, with angular resolution up to 1 arcmin. It includes bright and faint radio sources, Galactic synchrotron and Galactic freefree emissions. I have also developed a method to extract the faint cosmological 21-cm signal, heavily contaminated by foreground emissions and receiver noise. The method uses a cascade of two Wiener filters, in frequency domain and then, in angular domain. The first filter exploits the smoothness of the foreground emissions along the frequency, while the second filter exploits the angular correlations of the cosmological signal, due to the receiver noise is considered to be nearly uncorrelated between different directions. I have developed a studied the performance of a new imaging algorithm for lunar orbit interferometers. Such an instrument would be ideal for mapping the radio sky below 30 MHz, as it would be free from ionospheric perturbations, as well as electromagnetic interferences due to terrestrial emissions. I have shown that we make use of the precession of satellite orbital plane to solve the mirror symmetry problem, and exploit the linear mapping between the sky map and the measured visibilities, both in angular space and spherical harmonic space to reconstruct the sky map. The imaging algorithm handles the time-varying Moon's blockage over the whole sky field of view, which are not handled by existing imaging algorithms such as the WProjection and the W-Stacking. Finally, I have carried out a first analysis of the observational visibility data from the PAON-4 transit interferometer. I have evaluated the overall performance of the array in terms of system temperature and antenna response, and successfully calibrated the visibilities, determining both amplitude and phase of the complex gain terms, while correcting PAON-4 antennae pointing offsets. I have then reconstructed the sky map for a 10 degree strip around Cygnus A declination, from the cleaned calibrated PAON-4 data streams, applying the m-mode decomposition map-making algorithm in spherical harmonic space
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Graef, Leila Lobato. "Um modelo para decaimento da energia escura." Universidade de São Paulo, 2012. http://www.teses.usp.br/teses/disponiveis/43/43134/tde-08082012-150548/.
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Neste trabalho discutimos um modelo baseado em teoria de campos para descrever a energia escura, no qual ela é representada por uma partícula ultra-leve situada em um mínimo metaestável de um potencial. Mostramos que a energia escura neste modelo decai em matéria escura durante o tempo de vida do universo, amenizando o problema da coincidência.In the present work we discuss a field theory model in which dark energy is described by ultra-light particle situated at a metastable minimum of a potential. We show that dark energy in this model decays into dark matter during a time scale corresponding to the age of the universe, alleviating the coincidence problem.
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França, Junior Urbano Lopes. "Fenomenologia de modelos cosmológicos com campos escalares exponenciais /." São Paulo, 2004. http://hdl.handle.net/11449/132592.
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Orientador: Rogério RosenfeldBanca: Ruben Aldrovandi
Banca: Luís Raul Weber Abramo
Resumo: Nos últimos anos diversas evidências acumularam-se indicando que o universo é plano e dominado por alguma forma de energia escura, cuja pressão negativa está atualmente fazendo com que ele esteja em expansão acelerada. Vários modelos têm sido propostos para a energia escura, entre os quais destacam-se os modelos de quintessência, nos quais essa energia é modelada por um campo escalar. Neste trabalho analisamos alguns vínculos observacionais nos modelos de quintessência com potenciais exponenciais, e obtivemos limites para o espaço de parâmetros desses modelos no caso em que a quintessência está desacoplada dos demais componentes do universo e no caso em que ela está acoplada à partícula de matéria escura. No caso desacoplado, estudamos as soluções do tipo scaling, e mostramos que nesse regime, o único em que a quintessência exponencial desacoplada apresenta soluções cosmologicamente realísticas, esses modelos não podem ser considerados menos naturais que os demais potenciais de quintessência. Obtivemos ainda que o caso acoplado, assim como o desacoplado, também não resolve o problema da coincidência cósmica, e que a idade do universo nestes modelos é consideravelmente maior que no caso desacoplado, de modo que os limites na idade podem ser úteis para distinguir observacionalmente entre as quintessências acoplada e desacoplada
Abstract: During the last years many evidences are indicating that the universe is flat and dominated by some form of dark energy, whose negative pressure is currently driving its accelerated expansion. A plenty of models have been proposed, with special attention to the quintessence models, in which the dark energy is modelled by a scalar field. In this work we have analysed some observational constraints in the quintessence models with exponential potentials, and we have put limits on the parameter space in both coupled and uncoupled cases. In the uncoupled case, we have studied the scaling Solutions, and we have showed that in this regime, that is the only one in which the exponential uncoupled quintessence presents realistic Solutions, such models can not be considered less natural than others quintessence potentials. We have also obtained that in the case in which the quintessence is coupled to dark matter the cosmic coincidence problem can not be solved, and that the age for coupled models is considerably higher than the age for non-coupled models, in such a way that limits on the age can be useful in distinguishing between coupled and non-coupled models.
Mestre
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Zhao, Gang. "Dark world and the standard model." [College Station, Tex. : Texas A&M University, 2006. http://hdl.handle.net/1969.1/ETD-TAMU-1840.
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Farooq, Muhammad Omer. "Observational constraints on dark energy cosmological model parameters." Diss., Kansas State University, 2013. http://hdl.handle.net/2097/16623.
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Doctor of PhilosophyDepartment of Physics
Bharat Ratra
The expansion rate of the Universe changes with time, initially slowing (decelerating) when the universe was matter dominated, because of the mutual gravitational attraction of all the matter in it, and more recently speeding up (accelerating). A number of cosmological observations now strongly support the idea that the Universe is spatially flat (provided the dark energy density is at least approximately time independent) and is currently undergoing an accelerated cosmological expansion. A majority of cosmologists consider ``dark energy" to be the cause of this observed accelerated cosmological expansion. The ``standard" model of cosmology is the spatially-flat $\Lambda$CDM model. Although most predictions of the $\Lambda$CDM model are reasonably consistent with measurements, the $\Lambda$CDM model has some curious features. To overcome these difficulties, different Dark Energy models have been proposed. Two of these models, the XCDM parametrization and the slow rolling scalar field model $\phi$CDM, along with ``standard" $\Lambda$CDM, with the generalization of XCDM and $\phi$CDM in non-flat spatial geometries are considered here and observational data are used to constrain their parameter sets. In this thesis, we start with a overview of the general theory of relativity, Friedmann's equations, and distance measures in cosmology. In the following chapters we explain how we can constrain the three above mentioned cosmological models using three data sets: measurements of the Hubble parameter $H(z)$, Supernova (SN) apparent magnitudes, and the baryonic acoustic oscillations (BAO) peak length scale, as functions of redshift $z$. We then discuss constraints on the deceleration-acceleration transition redshift $z_{\rm da}$ using unbinned and binned $H(z)$ data. Finally, we incorporate the spatial curvature in the XCDM and $\phi$CDM model and determine observational constraints on the parameters of these expanded models.
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Bachega, Riis Rhavia Assis. "Vinculando modelos de energia escura com idade de galáxias em altos redshifts." Universidade de São Paulo, 2014. http://www.teses.usp.br/teses/disponiveis/43/43134/tde-27112014-233930/.
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Uma série de observações advindas da medida da distância de supernovas tipo IA, idade das estrelas mais antigas, anisotropias da radiação cósmica de fundo, entre outras, evidenciam que o universo está passando por uma fase de expansão acelerada. Essa expansão está sendo causada por uma componente misteriosa denominada energia escura, que representa cerca de $70\\%$ do conteúdo total do universo, e cuja natureza é desconhecida. Para descrever a energia escura vários modelos têm sido propostos, entre eles, podemos destacar a energia do vácuo (constante cosmológica) e um campo escalar dinâmico (quintessência). Também são considerados modelos em que a energia escura interage com outro componente misterioso, a matéria escura. Existem vários testes observacionais para vincular os parâmetros desses modelos. Nesta dissertação, exploraremos um método baseado na idade de galáxias em altos redshifts e na idade do universo, conhecido em inglês como lookback time.A number of observations arising from the measurement of distance of type IA Supernovae, age of oldest stars, anisotropy of cosmic microwave background, among others, show that the universe is undergoing a phase of accelerated expansion. This expansion is being caused by a mysterious component called dark energy, which represents about $70\\%$ of the total content of the universe, and whose nature is unknown. To describe the various dark energy models have been proposed, among them we highlight the vacuum energy (cosmological constant), and a dynamic scalar field (quintessence). Are also considered models in which dark energy interacts with another mysterious component, the dark matter. There are several observational tests to constraint the parameters of these models. In this dissertation, we explore a method based on age of galaxies at high redshift and the age of the universe, known as lookback time.
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Wang, Chao. "A model study of the dynamics of dark energy." Thesis, McGill University, 2012. http://digitool.Library.McGill.CA:80/R/?func=dbin-jump-full&object_id=106572.
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Observational facts indicate that the expansion of the universe is accelerating, rather than decelerating, because 73% of the total energy density of the universe is a "dark energy" with strong negative pressure, ω < −1/3. In this thesis, we introduce a dynamical dark energy model with dilatational symmetry, which contains two scalar fields coupled to gravity. Because of the dilatational symmetry, there is no cosmological constant Λ in the Lagrangian, and, instead, two scalar fields generate the dark energy, evolving slowly in time. At early times, the system is in the slow roll regime, corresponding to Higgs inflation due to the Higgs field. At late times, the dynamical dark energy dominates the universe and eventually behaves just like the cosmological constant, and the universe becomes exponentially expanding with the scale factor a(t) ∝ exp{Ht}. The numerical results from solving the dynamic equations of the system agree well with the observational facts, which indicates that our model gives a good description of the universe. At the end of the thesis, we consider the one-loop corrections to our model, and show that they do not alter the classical results in any significant way.Les observations actuelles de l'expansion de l'univers indiquent une accéleration decette expansion due à 'l'énergie sombre', qui compte pour 73% de la densité d'énergie totalle de l'univers et qui se comporte comme un fluide avec une pression négative, ω < −1/3. Cette thèse présente un modèle dynamique d'énergie sombre invariant sous une symétrie de dilatation comprenant deux champs scalaires couplés à la gravitation. La constante cosmologique n'est pas présente dans ce modèle, de par la symétrie de dilatation; les champs scalaires génèrent une énergie sombre évoluant dans le temps. Dans l'univers primordial, le système se situe dans le régime d'évolution lente correspondant à l'inflation cosmolgique due au champ de Higgs. L'énergie sombre dynamique agit ultérieurement sur l'évolution de l'univers comme une constante cosmologique; le facteur d'échelle de l'univers accroit de manière exponentielle a(t) ∝ eHt. Les simulations numériques concordent très bien avec les observations actuelles. Les perturbations quantiques de premier ordre sont ensuite calculées, et justifient la validité des résultats obtenus de manière classique.
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Marra, Valerio. "A Back-Reaction Approach to Dark Energy." Doctoral thesis, Università degli studi di Padova, 2008. http://hdl.handle.net/11577/3425542.
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This thesis is mainly about how to set up and carry out in a physically meaningful way the idea of back-reaction, which is an alternative theory to a theory where dark energy is fundamental.
There are, broadly speaking, two distinct approaches. One is focused on how cosmological observables are affected by inhomogeneities, while the other is focused on a theoretical description of the inhomogeneous universe by means of a mean-field description. Both approaches, however, share the idea of smoothing out inhomogeneities. We developed this duality in the interpretation of the back-reaction by means of toy models based on the Lemaitre-Tolman-Bondi solution of Einstein's equations.
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Alles, Alexandre. "Inhomogeneous cosmology : an answer to the Dark Matter and Dark Energy problems?" Thesis, Lyon 1, 2014. http://www.theses.fr/2014LYO10165/document.
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Le Modèle Standard de la cosmologie décrit la formation des structures à grande échelle dans l'Univers récent dans un cadre quasi–newtonien. Ce modèle requiert la présence de composantes inconnues, la Matière Noire et l'Énergie Noire, afin de vérifier correctement les observations. Ces deux quantités représentent à elles seules près de 95% du contenu de l'Univers. Bien que ces composantes sombres soient activement recherchées par la communauté scientifique, il existe plusieurs alternatives qui tentent de traiter le problème des structures à grande échelle. Les théories inhomogènes décrivent l'impact des fluctuations cinématiques sur le comportement global de l'Univers. D'autres théories proposent également d'aller au-delà de la relativité générale. Durant cette thèse, j'ai mis au point des éléments clés d'une théorie lagrangienne totalement relativiste de la formation des structures. Supposant un feuilletage particulier de l'espace–temps j'ai résolu le système d'équations du premier ordre afin d'obtenir des solutions décrivant l'évolution de la matière dans un espace à la géométrie perturbée. J'ai également développé un schéma de résolution pour les ordres supérieurs de perturbation ainsi que leurs équivalent newtoniens. Une autre partie de ce travail de thèse consiste en le développement de quelques applications directes : la description d'un Univers silencieux ou l'hypothèse de courbure de Weyl et le problème de 'entropie gravitationnelle. Les objectifs à plus ou moins court terme seraient d'obtenir la description d'observables physiques and le développement d'autres applications. Cette étape de développement sera une interaction entre approches théorique et numérique et requerra de se rapprocher fortement des observateursThe standard model of cosmology describes the formation of large scale structures in the late Universe within a quasi–Newtonian theory. This model requires the presence of unknown compounds of the Universe, Dark Matter and Dark Energy, to properly fit the observations. These two quantities, according to the Standard Model, represent almost 95% of the content of the Universe. Although the dark components are searched for by the scientific community, there exist several alternatives which try to deal with the problem of the large scale structures. Inhomogeneous theories describe the impact of the kinematical fluctuations on the global behaviour of the Universe. Or some theories proposed to go beyond general relativity. During my Ph.D. thesis, I developed key–elements of a fully relativistic Lagrangian theory of structure formation. Assuming a specific space–time slicing, I solved the first order system of equations to obtain solutions which describe the matter evolution within the perturbed geometry, and I developed higher order schemes and their correspondences with the Lagrangian perturbation solutions in the Newtonian approach. I also worked on some applications of these results like the description of a silent Universe or the Weyl curvature hypothesis and the problem of gravitational entropy. Further objectives are the description of physical observables and the development of direct applications. Next step of the development is an interaction between theoretical and numerical approaches, a study which would require strong cooperation with observers
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Smer, Barreto Vanessa Stephanie Emilia. "Probing of dark energy properties in the Universe using astrophysical observations." Thesis, University of Edinburgh, 2017. http://hdl.handle.net/1842/28956.
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The astrophysical data of the last two decades have allowed cosmologists to conclude that the present Universe is accelerating. The research carried out to find the origin of this phenomenon has led to the creation of a vast number of dark energy and modified gravity theories, of which the simplest is the ˄CDM model. The latter is, however, plagued with very difficult problems awaiting a solution. The work here presented seeks to contribute to the discussion of the possible explanation for the Cosmos' acceleration and other important questions in modern cosmology using the newest astrophysical observations available. This thesis starts by exploring a dark energy model dubbed thawing quintessence which is characterised by allowing a non constant ratio of pressure to density for dark energy that is however still close to -1 for most of the cosmological evolution, shifting away from this value when the domination of the radiation and matter components fades away. The findings are the most up-to-date constraints for which this model gives a viable theory for dark energy, including a bound on the equation of state at present of w < -0:88. This exact approach was contrasted with the use of an approximate equation-of-state parametrisation for thawing theories. The analysis also includes different parametrisation choices, and comments on the accuracy of the constraints imposed by CMB anisotropies alone. Next, the cosmology of hybrid metric-Palatini gravity is presented. This is a type of Modified Gravity theory in which the Lagrangian density for the gravitational action is a function of the Ricci scalars of both the connection and the metric. The background evolution of two models of this kind is examined explicitly showing the recovery of standard General Relativity at late times. The maximum deviation from the gravitational constant G at early times is constrained using a combination of geometrical data, finding it to be around 1%. A designer scenario, also introduced under the hybrid metric-Palatini formulation, is then used to explore to what extent early modifications of gravity, which become significant after recombination but then decay towards the present, can be constrained by current and future cosmological observations. This model is embedded in the effective field theory description of Horndeski scalar-tensor gravity with an early-time decoupling of the gravitational modification. Applying cosmological data, the constraints on the early-time deviations from General Relativity are obtained. These are dependent on the redshift at which the oscillations in the slip between the gravitational potentials are turned on. For zon = 1000, the deviation from Einstein's theory is ≤ 10-2 with 95% confidence. An explanation of the effect that these divergences have on the CMB power spectrum are discussed, as well as the effect that future 21 cm survey data will have on this study. The last part of this work is a move towards inflation, the early epoch of accelerated expansion undergone by the Universe. Here a parametrisation of the acceleration trajectory is investigated with the aim of measuring the rolling of the inflaton corresponding to the value of the tensor-to-scalar ratio r to be compared with future observations. Considering five ln ε amplitudes and 14 e-foldings, it was found that the posterior distribution of (r,∆Φ) is in very good agreement with Lyth's bound. The analysis included a histogram depiction of the latter result, from which later a minimum constraint on ∆ϕ for each of the bins was found. These outcomes constitute the intermediate step of this project which will be made more accurate by extending it to ~ 50 e-folds, a larger set of cosmological parameters and observational bounds that are restrictive on small scales.
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Sharma, Arjun. "Placing Limits on Experimental Signatures of Dark Matter Model Predictions." Thesis, The University of Chicago, 2018. http://pqdtopen.proquest.com/#viewpdf?dispub=10807985.
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In this work, we consider two different models of dark matter and set limits on results of experiments. One is a dynamic dark matter scenario where we put limits on parameters observable by experiments DAMA and XMASS through nuclear recoil of detector atoms (direct detection). The second is a case of dark matter annihilation into positrons and electrons and the signal this would produce on measured values of positron flux and ratio of electron to positron (indirect detection). The values of these quantities as measured by FERMI and PAMELA experiments are observed and an explanation using a dark matter annihilation is presented vs astrophysical sources of particles.
We explore a dynamic dark matter scenario with an ensemble of dark matter particles that starts at m0 and spans a comb of particles separated by jδΔ m. We verify the model by using Δm = ∞ and comparing the predictions to a non dynamic model for the same mass m0. We then observe the wider set of possibilities available with the dynamic dark matter model compared with the single mass case vis a vis constraints set by NaI and Xe detectors published by the DAMA and XMASS collaborations and check for validity of model against these measurements.
The Fermi experiment has measured the cosmic ray electron+positron spectrum and positron fraction [фe+/(фe++e−)], and PAMELA has measured the positron fraction with better precision. While the majority of cosmic ray electrons and positrons are of astrophysical origin, there may also be a contribution from dark matter annihilation in the galactic halo. The upcoming results of the AMS experiment will show measurements of these quantities with far greater precision. One dark matter annihilation scenario is where two dark matter particles annihilate directly to e + and e− final states. In this article, we calculate the signature “bumps” in these measurements assuming a given density profile (NFW profile). If the dark matter annihilates to electrons and positrons with a cross section σv ∼ 10−26 cm3/s or greater, this feature may be discernible by AMS. However, we demonstrate that such a prominent spectral feature is already ruled out by the relative smoothness of the positron + electron cosmic ray spectrum as measured by Fermi. Hence we conclude that such a feature is undetectable unless the mass is less than ∼40 GeV.
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Zunckel, Caroline Louise. "Beyond the standard cosmological model : dark energy, massive neutrinos and statistical isotropy." Thesis, University of Oxford, 2008. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.670059.
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Tekola, Abiy G. "Spherically symmetric dark energy structures in the context of Chaplygin gas model." Master's thesis, University of Cape Town, 2006. http://hdl.handle.net/11427/6518.
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Includes bibliographical references (leaves 42-43).This paper investigates the existence of spherically symmetrical dark energy structures under the context of Chaplygin gas. A scaling solution of the form r -2/3 is found for the density and then we calculated the corresponding rotational curve and it turns out to be unrealistic implying that such objects don't exist. Finally we modified the equation of state of the Chaplygin gas to an equation of state of the form P = (j 2 P - A and compared p with observational data to see to what physical extent this equation works and it isdetermined that it works as far as a couple of hundred Mpc while the physical length of galaxies is in Kpc. implying the modified Chaplygin equation fits the observed rotational curves.
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Boediarto, Feby. "Democracy in the Dark: An Energy Democracy Model Centering Property and People." Scholarship @ Claremont, 2017. http://scholarship.claremont.edu/pitzer_theses/81.
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The United States’ electric macro-grid provides electricity for all people to sustain our lifestyle. The current governing institutions that generate our electricity limit community representation, causing procedural injustice particularly to communities of color. This thesis is a contribution to the Energy Democracy literature, describing a community-based electricity model that includes two components: property and people. I argue to include an in-depth study of John Locke’s theories on property, in addition to Elinor Ostrom’s Institutional Analysis and Development Framework to promote local knowledge in understanding how physical space and governing bodies strengthen the Energy Democracy movement. In addition, I utilize the works from Karl Marx and Grace Lee Boggs to describe the process of local self-reliance to community empowerment. This Energy Democracy approach centering property and people aims to revolutionize a system that promotes equity and democracy.
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Tocchini-Valentini, Domenico. "Beyond the standard cosmological model : primordial power spectrum and dark energy coupled to neutrinos." Thesis, University of Oxford, 2006. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.432334.
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Lopes, Rafael Christ de Castro. "Estudo do raio de turnaround em teorias f(R)." Universidade de São Paulo, 2019. http://www.teses.usp.br/teses/disponiveis/43/43134/tde-21032019-154839/.
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Nós investigamos o raio de turnaround, a distância do centro da estrutura cósmica até a casca que está se descolando do fluxo de Hubble em um dado tempo, no contexto do modelo de colapso esférico, tanto em Relatividade Geral e em Gravidade Modificada, em particular no cenário f(R) chamado de modelo de Hu-Sawicki. O próximo passo foi investigar a relação entre este raio e a massa de virial de estruturas cósmicas no contexto do modelo LCDM e no modelo f(R) de gravidade modificada.We investigate the turnaround radius, the distance from the center of the cosmic structure to the shell that is detaching from the Hubble flow at a given time, in the context of the spherical collapse model, both in General Relativity and in modified gravity, in particular f(R) scenarios -- namely the Hu-Sawicki model. The next step was to investigate the relationship between that radius and the virial mass of cosmic structures in the context of LCDM model and in an f(R) model of modified gravity.
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Leonard, Catherine Danielle Bartlett. "Beyond the standard cosmological paradigm with weak gravitational lensing." Thesis, University of Oxford, 2016. https://ora.ox.ac.uk/objects/uuid:15c2979e-f085-4836-97be-6890740ed4ba.
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Next-generation cosmological surveys will demand an unprecedented understanding of the interplay between theoretical and observational aspects of weak gravitational lensing. This thesis presents a study of the parameter degeneracies and theoretical uncertainties which will affect weak lensing tests of cosmology beyond the standard paradigm. In particular, tests of alternative theories of gravity and of spatial curvature are considered. First, by considering linear-order departures from the standard gravitational theory of general relativity, a novel expression is derived for the weak lensing convergence power spectrum under alternative theories of gravity. Using this expression, degeneracies between gravitational parameters in weak lensing observations are explored, first with a focus on scale-independent parameterisations of gravity, then considering new physical scales introduced by alternative theories. The degeneracy-breaking offered by the combination of weak lensing and redshift-space distortions is shown to be robust to the time-dependence of the functions parameterising modified gravity. Next, the gravity-testing statistic EG is investigated, and a new theoretical expression for its observationally-motivated definition is presented. The theoretical uncertainty of EG is compared to forecast statistical errors, and found to be significant in the case of a more futuristic measurement. Predictions are then computed for EG under deviations from general relativity, and the ongoing utility of EG as a probe of gravity is discussed. Finally, an investigation is made of the potential for measuring or constraining the spatial curvature using weak lensing and complementary observables. The predicted constraint on the spatial curvature is forecast for a suite of upcoming surveys, and the effect of including parameters which may be degenerate with the spatial curvature is explored. It is found that upcoming observations are likely to constrain spatial curvature at a 10⁻³ level, but not to reach the best-case constraint of ~10⁻⁴.
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Maniyar, Abhishek Sanjay. "From the CMB to CIB : dusty star formation, dark energy and kSZ." Thesis, Aix-Marseille, 2019. http://theses.univ-amu.fr.lama.univ-amu.fr/190919_MANIYAR_759uunye462vklkb421iixa572jct_TH.pdf.
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Le fond diffus infrarouge (CIB) provient de l'émission IR cumulée des galaxies sur toute l'histoire de l'Univers. Ainsi, le CIB sonde la formation et l'évolution des galaxies sur une grande gamme de décalage vers le rouge. Dans cette thèse, nous utilisons les anisotropies du CIB pour: i) Mesurer l'histoire de la formation des étoiles de l'Univers et le biais effectif des halos de matière noire hébergeant les galaxies CIB jusqu'à un décalage rouge élevé. En utilisant ces mesures, nous calculons la masse typique de ces halos de matière noire, sur une grande gamme de décalage vers le rouge. ii) En utilisant le CIB comme traceur de la structure à grande échelle, la corrélation croisée avec le CMB fournit une sonde alternative de l'énergie noire. Nous montrons que le CIB, extrait sur une grande fraction du ciel, peut fournir la meilleure mesure de l'effet ISW. En utilisant un formalisme matriciel de Fisher, nous prédisons l'amélioration des contraintes sur les paramètres cosmologiques en utilisant l'ISW mesuré avec le CIB. iii) Mesurer le spectre de puissance de l'effet Sunyaev-Zel'dovich cinétique (kSZ) caché dans les données du CMB. Nous améliorons les analyses existantes en combinant les mesures du CIB (de Planck/HFI et Herschel/SPIRE) et les observations de Planck, SPT et ACT pour étendre la gamme des échelles spatiales et des fréquences afin de faciliter la mesure du kSZ. Nous développons un nouveau modèle pour le CIB (pour pouvoir tenir compte des petites échelles spatiales), et modélisons de façon cohérente l'effet SZ thermique (tSZ) et la corrélation CIBxtSZ. Ceci est nécessaire pour séparer avec précision ces différentes composantes dans le spectre de puissanceThe CIB is the cumulative infrared emission from all the galaxies throughout cosmic history. Its distinct frequency-redshift dependence allows to probe a large span of redshifts. In this thesis, we utilise the CIB anisotropies detected by the Planck satellite to:i) Measure the star formation history of the Universe and the effective bias of the dark matter halos hosting the CIB galaxies to a high redshift. Using these measurements, we calculate the typical mass of the host dark matter halos for the CIB galaxies at different times.ii) Using the CIB as a tracer of the large scale structure, the cross-correlation with the CMB provides with an alternative probe of the dark energy. We showed that the CIB, extracted on a large fraction of the sky, may provide the best Integrated Sachs Wolf measurement (in terms of S/N ratio). Using a Fisher matrix formalism, we also predict the improvement on the constraints on the cosmological parameters using the ISW measured with this technique. We cross-correlate the best available maps of the CIB and the CMB and find that the dust residuals in the CIB maps are too high to detect the ISW through this method.iii) Measure the kinetic Sunyaev-Zel'dovich (kSZ) power spectrum hidden in the CMB power spectrum. We improve upon the existing analysis by combining the CIB measurements (from Planck/HFI and Herschel/SPIRE) and multi-frequency observations by Planck, SPT and ACT to extend the range of scales and frequencies to facilitate the kSZ measurement. We develop a power spectrum analysis based on physically motivated but simplistic and consistent models of foreground components (CIB, tSZ, tSZxCIB) to accurately separate the kSZ from the CMB
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Ali, Sahba Yahya Hamid. "Probing the expansion history of the universe using upernovae and Baryon Acoustic Oscillations." University of the Western Cape, 2016. http://hdl.handle.net/11394/5054.
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Philosophiae Doctor - PhDThe standard model of cosmology (the ɅCDM model) has been very successful and is compatible with all observational data up to now. However, it remains an important task to develop and apply null tests of this model. These tests are based on observables that probe cosmic distances and cosmic evolution history. Supernovae observations use the so-called `standard candle' property of SNIa to probe cosmic distances D(z). The evolution of the expansion rate H(z) is probed by the baryon acoustic oscillation (BAO) feature in the galaxy distribution, which serves as an effective `standard ruler'. The observables D(z) and H(z) are used in various consistency tests of ɅCDM that have been developed. We review the consistency tests, also looking for possible new tests. Then the tests are applied, first using existing data, and then using mock data from future planned experiments. In particular we use data from the recently commissioned Dark Energy Survey (DES) for SNIa. Gaussian Processes, and possibly other non-parametric methods, used to reconstruct the derivatives of D (z) and H (z) that are needed to apply the null tests of the standard cosmological model. This allows us to estimate the current and future power of observations to probe the ɅCDM model, which is the foundation of modern cosmology. In addition, we present an improved model of the HI galaxy number counts and bias from semi-analytic simulations, and we use it to calculate the expected yield of HI galaxies from surveys with a variety of phase 1 and 2 SKA configurations. We illustrate the relative performance of the different surveys by forecasting errors on the radial and transverse scales of the BAO feature. We use the Fisher matrix method to estimate the error bars on the cosmological parameters from future SKA HI galaxy surveys. We find that the SKA phase 1 galaxy surveys will not contend with surveys such as the Baryon Oscillation Spectroscopic Survey (BOSS) whereas the full "billion galaxy survey" with SKA phase 2 will deliver the largest dark energy Figure of Merit of any current or future large-scale structure survey.
South African Square Kilometre Array Project (SKA) and German Academic Exchange Service (DAAD)
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Umiltà, Caterina. "Cosmological predictions for a scalar tensor dark energy model by a dedicated Einstein-Boltzmann code." Master's thesis, Alma Mater Studiorum - Università di Bologna, 2014. http://amslaurea.unibo.it/6580/.
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Vlcek, Brian J. "Beyond the standard model| Ihc phenomenology, cosmology from post-inflationary sources, and dark matter physics." Thesis, The University of Wisconsin - Milwaukee, 2014. http://pqdtopen.proquest.com/#viewpdf?dispub=3613650.
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It is the goal of this dissertation to demonstrate that beyond the standard model, certain theories exist which solve conflicts between observation and theory -- conflicts such as massive neutrinos, dark matter, unstable Higgs vacuum, and recent Planck observations of excess relativistic degrees of freedom in the early universe. Theories explored include a D-brane inspired construct of U(3) × Sp(1) × U(1) × U(1) extension of the standard model, in which we demonstrate several possible observables that may be detected at the LHC, and an ability to stabilize the Higgs mechanism. The extended model can also explain recent Planck data which, when added to HST data gives an excess of relativistic degrees of freedom of Δ N = 0.574 ± 0.25 above the standard result. Also explored is a possible non-thermal dark matter model for explanation of this result. Recent observations of Fermi bubble results indicate a signal of a 50 GeV dark matter particle annihilating into b b-bar, with a thermally averaged annihilation cross section corresponding to <σ v> = 8 × 10
(-27) cm
3/s, spurs interestin a Higgs portal model suggested by Steven Weinberg. Other implications of this model are also explored such as its ability to explain dark matter direct detection results along with LHC Higgs data, and Planck data. Particle physics is complimented by possible stochastic gravitational wave searches for which a model of second order global phase transitions is explored. These transitions generate gravitational wave spectra with amplitudes of order Ω(gw) h
2 = 10
(-24) - 10
(-15). Furthermore, techniques into such calculationsare investigated in hopes to improve the stability required in such lattice simulations.
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Hierro, Rodriguez Ignacio Miguel. "Scalars beyond the Standard Model: Composite Higgs, dark matter and neutrino masses." Doctoral thesis, Università degli studi di Padova, 2017. http://hdl.handle.net/11577/3426319.
Full textAbstract:
This thesis deals with Composite Higgs (CH) models, dark matter and neutrino masses. In CH models, the Higgs is a pseudo-Goldstone boson of a high-energy strong dynamics. We construct CP-even and CP-odd bosonic effective chiral Lagrangian for a generic symmetric coset G/H. Assuming that the only sources of custodial symmetry are the ones present in the SM, we study the projection of this Lagrangian into the low-energy SM chiral Lagrangian. This is applied in three particular scenarios: the original SU(5)/SO(5) Georgi-Kaplan model, the minimal custodialpreserving SO(5)/SO(4) model and the minimal SU(3)/(SU(2)×U(1)) model, which intrinsically breaks custodial symmetry. We furthermore consider an extension of the Standard Model involving two new scalar particles around the TeV scale: a singlet neutral scalar φ, to be eventually identified as the Dark Matter candidate, plus a doubly charged SU(2)L singlet scalar, S++, that can be the source for the nonvanishing neutrino masses and mixings. Assuming an unbroken Z_2 symmetry in the scalar sector, under which only the additional neutral scalar φ is odd, we write the most general (renormalizable) scalar potential. This model may be regarded as a possible extension of the conventional Higgs portal Dark Matter scenario which in addition accounts for neutrino masses and mixings. This framework cannot completely explain the observed positron excess. However a softening of the discrepancy observed in conventional Higgs portal framework can be obtained, especially when the scale of new physics responsible, for generating neutrino masses and lepton number violating processes, is around 2 TeV.Questa tesi si occupa di studiare modelli di Higgs Composto (HC), materia oscura e masse dei neutrini. In modelli di tipo HC, lo scalare di Higgs è uno pseudo-bosone di Goldstone associato che origina dalla rottura di una simmetria forte ad alta energia. Nella tesi costruiamo la Lagrangiana chirale bosonica effettiva, per un generico coset simmetrico G/H, derivando esplicitamente tutti gli operatori (sia CP-even che CP-odd) che appaiono fino a quattro derivate. Supponendo che l’uniche fonte di rottura di simmetria custodial siano quelle già presente nel Modello Standard (MS), studiamo la proiezione di questa Lagrangiana sulla Lagrangiana chirale di bassa energia del MS. Particolareggiamo questo studio considerando tre scenari particolari: il modello originale di Georgi-Kaplan SU(5)/SO(5), il modello minimale con simmetria custodial, SO(5)/SO(4), ed il modello minimale senza simmetria custodial, SU(3)/(SU(2) × U(1)). Nella tesi consideriamo inoltre unestensione del MS che coinvolge due nuove particelle scalari con massa alla scala TeV: un singoletto scalare neutro φ, che sarà poi identificato come candidato di materia oscura e un singoletto di SU(2)L scalare con carica q = 2, S++, che può essere la fonte per le masse e del mixing dei neutrini. Supponendo l’esistenza di una simmetria Z_2 nel settore scalare, sotto la quale solo φ è dispari, scriviamo il potenziale scalare (rinormalizzabile) più generale possibile. Il modello si può vedere come una possible estensione dei modelli con Higgs Portal in cui si tiene anche conto del meccanismo con cui generare le masse e i mixings dei neutrini. Il modello da noi studiato, pur predice un eccesso di positroni, non tale tuttavia da poter spiegare l’eccesso di positroni sperimentalmente osservato. Pur tuttavia si possono ottenere dei limiti meno stringenti rispetto ai normali modelli di Higgs Portal, in particolare se la scala della nuova fisica, responsabile della generazione delle masse dei neutrini e dei processi che violano il numero leptonico, è intorno ai 2 TeV.
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Hallsjö, Sven-Patrik. "Search for Dark Matter in the Upgraded High Luminosity LHC at CERN : Sensitivity of ATLAS phase II upgrade to dark matter production." Thesis, Linköpings universitet, Institutionen för fysik, kemi och biologi, 2014. http://urn.kb.se/resolve?urn=urn:nbn:se:liu:diva-107583.
Full textAbstract:
The LHC at CERN is now undergoing a set of upgrades to increase the center of mass energy for the colliding particles to be able to explore new physical processes. The focus of this thesis lies on the so called phase II upgrade which will preliminarily be completed in 2023. After the upgrade the LHC will be able to accelerate proton beams to such a velocity thateach proton has a center of mass energy of 14 TeV. One disadvantage of the upgrade is that it will be harder for the atlas detector to isolate unique particle collisions since more and more collisions will occur simultaneously, so called pile-up. For 14 TeV there does not exist a full simulation of the atlas detector. This thesis instead uses data from Monte Carlo simulations for the particle collisions and then uses so called smearing functions to emulate the detector responses. This thesis focuses on how a mono-jet analysis looking for different wimp models of dark matter will be affected by this increase in pile-up rate. The signal models which are in focus are those which try to explain dark matter without adding new theories to the standard model or QFT, such as the effective theory D5 operator and light vector mediator models. The exclusion limits set for the D5 operators mass suppression scale at 14 TeV and 1000 fb-1are 2-3 times better than previous results at 8 TeV and 10 fb-1. For the first time limits have been set on which vector mediator mass models can be excluded at 14 TeV.