Kiribilen kosmologia kuantikorako sarrera

Gradu amaierako lan hau kiribilen kosmologia kuantikorako sarrera bat da. Lan honek 4 kapi- tulu ditu. Lehenengoan, sarrera bezala grabitazio kuantikoak izan duen bilakaera historikoa jaso da, halako teoria bat garatzeko motibazioak eta zailtasunak, eta honen garapenean kosmologia kuantikoak duen papera azalduz. Lanean, oro har, grabitazio kuantikoaren teoria bat eraikitzeko formalismo “kanonikoa” jarraitu da, alegia, erlatibitate orokorraren formulazio hamiltondarra era- biliz teoria kuantikoa garatzea. Bigarren kapituluan grabitazioaren teoria klasikoaren formulazio hamiltondarra garatu da, lehenik Arnowitt-Deser-Misner formalismoaren (Einstein-en geometro- dinamika bezala ere ezaguna denaren) bidez eta ondoren Ashtekar-en aldagaiak erabiliz. Bietan hamiltondar guztiz lotua lortzen da, hots, loturen konbinazio lineala den hamiltondarra. Lotu- ren bidezko formulazio hauen kuantizazioaren eta kribilen adierazpenaren oinarrizko aspektuak jaso dira bigarren kapituluan. Hirugarren kapituluan kosmologiaren teoria klasikoa Friedmann- Lemaˆ ıtre-Robertson-Walker metrika laua erabiliz azaltzen da era laburrean lehenik, eta ondoren Wheeler-DeWitt teoria kuantikoa eta kiribilen kosmologia kuantikoa eta hauek erabiliz lorturiko zenbait emaitza aipatzen dira. Azkenik, ondorioen atalarekin amaitzen da lana. Lana euskaraz idatzita dago.

Consequences of Supersymmetry in the Early Universe

Currently, we live in an era characterized by the completion and first runs of the LHC accelerator at CERN, which is hoped to provide the first experimental hints of what lies beyond the Standard Model of particle physics. In addition, the last decade has witnessed a new dawn of cosmology, where it has truly emerged as a precision science. Largely due to the WMAP measurements of the cosmic microwave background, we now believe to have quantitative control of much of the history of our universe. These two experimental windows offer us not only an unprecedented view of the smallest and largest structures of the universe, but also a glimpse at the very first moments in its history. At the same time, they require the theorists to focus on the fundamental challenges awaiting at the boundary of high energy particle physics and cosmology. What were the contents and properties of matter in the early universe? How is one to describe its interactions? What kind of implications do the various models of physics beyond the Standard Model have on the subsequent evolution of the universe? In this thesis, we explore the connection between in particular supersymmetric theories and the evolution of the early universe. First, we provide the reader with a general introduction to modern day particle cosmology from two angles: on one hand by reviewing our current knowledge of the history of the early universe, and on the other hand by introducing the basics of supersymmetry and its derivatives. Subsequently, with the help of the developed tools, we direct the attention to the specific questions addressed in the three original articles that form the main scientific contents of the thesis. Each of these papers concerns a distinct cosmological problem, ranging from the generation of the matter-antimatter asymmetry to inflation, and finally to the origin or very early stage of the universe. They nevertheless share a common factor in their use of the machinery of supersymmetric theories to address open questions in the corresponding cosmological models.

Aspects of Inflationary Models at Low Energy Scales

Cosmological inflation is the dominant paradigm in explaining the origin of structure in the universe. According to the inflationary scenario, there has been a period of nearly exponential expansion in the very early universe, long before the nucleosynthesis. Inflation is commonly considered as a consequence of some scalar field or fields whose energy density starts to dominate the universe. The inflationary expansion converts the quantum fluctuations of the fields into classical perturbations on superhorizon scales and these primordial perturbations are the seeds of the structure in the universe. Moreover, inflation also naturally explains the high degree of homogeneity and spatial flatness of the early universe. The real challenge of the inflationary cosmology lies in trying to establish a connection between the fields driving inflation and theories of particle physics. In this thesis we concentrate on inflationary models at scales well below the Planck scale. The low scale allows us to seek for candidates for the inflationary matter within extensions of the Standard Model but typically also implies fine-tuning problems. We discuss a low scale model where inflation is driven by a flat direction of the Minimally Supersymmetric Standard Model. The relation between the potential along the flat direction and the underlying supergravity model is studied. The low inflationary scale requires an extremely flat potential but we find that in this particular model the associated fine-tuning problems can be solved in a rather natural fashion in a class of supergravity models. For this class of models, the flatness is a consequence of the structure of the supergravity model and is insensitive to the vacuum expectation values of the fields that break supersymmetry. Another low scale model considered in the thesis is the curvaton scenario where the primordial perturbations originate from quantum fluctuations of a curvaton field, which is different from the fields driving inflation. The curvaton gives a negligible contribution to the total energy density during inflation but its perturbations become significant in the post-inflationary epoch. The separation between the fields driving inflation and the fields giving rise to primordial perturbations opens up new possibilities to lower the inflationary scale without introducing fine-tuning problems. The curvaton model typically gives rise to relatively large level of non-gaussian features in the statistics of primordial perturbations. We find that the level of non-gaussian effects is heavily dependent on the form of the curvaton potential. Future observations that provide more accurate information of the non-gaussian statistics can therefore place constraining bounds on the curvaton interactions.

Measuring the Cosmic Microwave Background : Topics along the analysis pipeline

The first quarter of the 20th century witnessed a rebirth of cosmology, study of our Universe, as a field of scientific research with testable theoretical predictions. The amount of available cosmological data grew slowly from a few galaxy redshift measurements, rotation curves and local light element abundances into the first detection of the cos- mic microwave background (CMB) in 1965. By the turn of the century the amount of data exploded incorporating fields of new, exciting cosmological observables such as lensing, Lyman alpha forests, type Ia supernovae, baryon acoustic oscillations and Sunyaev-Zeldovich regions to name a few. -- CMB, the ubiquitous afterglow of the Big Bang, carries with it a wealth of cosmological information. Unfortunately, that information, delicate intensity variations, turned out hard to extract from the overall temperature. Since the first detection, it took nearly 30 years before first evidence of fluctuations on the microwave background were presented. At present, high precision cosmology is solidly based on precise measurements of the CMB anisotropy making it possible to pinpoint cosmological parameters to one-in-a-hundred level precision. The progress has made it possible to build and test models of the Universe that differ in the way the cosmos evolved some fraction of the first second since the Big Bang. -- This thesis is concerned with the high precision CMB observations. It presents three selected topics along a CMB experiment analysis pipeline. Map-making and residual noise estimation are studied using an approach called destriping. The studied approximate methods are invaluable for the large datasets of any modern CMB experiment and will undoubtedly become even more so when the next generation of experiments reach the operational stage. -- We begin with a brief overview of cosmological observations and describe the general relativistic perturbation theory. Next we discuss the map-making problem of a CMB experiment and the characterization of residual noise present in the maps. In the end, the use of modern cosmological data is presented in the study of an extended cosmological model, the correlated isocurvature fluctuations. Current available data is shown to indicate that future experiments are certainly needed to provide more information on these extra degrees of freedom. Any solid evidence of the isocurvature modes would have a considerable impact due to their power in model selection.

'Someone to welcome you home' : Infertility, medicines and the Sukuma-Nyamwezi

This study Someone to Welcome you home: Infertility, medicines and the Sukuma-Nyamwezi , looks into the change in the cosmological ideology of the Sukuma-Nyamwezi of Tanzania and into the consequences of this change as expressed through cultural practices connected to female infertility. This analysis is based on 15 months of fieldwork in Isaka, in the Shinyanga area. In this area the birth rate is high and at the same time infertility is a problem for individual women. The attitudes connected to fertility and the attempts to control fertility provide a window onto social and cultural changes in the area. Even though the practices connected to fertility seem to be individualized the problem of individual women - the discourse surrounding fertility is concerned with higher cosmological levels. The traditional cosmology emphasized the centrality of the chief as the source of well-being. He was responsible for rain and the fertility of the land and, thus, for the well-being of the whole society. The holistic cosmology was hierarchical and the ritual practices connected to chiefship which dealt with the whole of the society were recursively applied at the lower levels of hierarchy, in the relationships between individuals. As on consequence of changes in the political system, the chiefship was legally abolished in the early years of Independence. However, the holistic ideology, which was the basis of the chiefship, did not disappear and instead acquired new forms. It is argued that in African societies the common efflorence of diviner-healers and witchcraft can be a consequence of the change in the relationship between the social reality and the cosmological ideology. In the Africanist research the increase in the numbers of diviner-healers and witchcraft is usually seen as a consequence of individualism and modernization. In this research, however, it is seen as an altered form of holism, as a consequence of which the hierarchical relations between women and men have changed. Because of this, the present-day practices connected to reproduction pay special attention to the control of women s sexuality.

Primordial Perturbations from a Self-interacting Curvaton

Inflation is a period of accelerated expansion in the very early universe, which has the appealing aspect that it can create primordial perturbations via quantum fluctuations. These primordial perturbations have been observed in the cosmic microwave background, and these perturbations also function as the seeds of all large-scale structure in the universe. Curvaton models are simple modifications of the standard inflationary paradigm, where inflation is driven by the energy density of the inflaton, but another field, the curvaton, is responsible for producing the primordial perturbations. The curvaton decays after inflation as ended, where the isocurvature perturbations of the curvaton are converted into adiabatic perturbations. Since the curvaton must decay, it must have some interactions. Additionally realistic curvaton models typically have some self-interactions. In this work we consider self-interacting curvaton models, where the self-interaction is a monomial in the potential, suppressed by the Planck scale, and thus the self-interaction is very weak. Nevertheless, since the self-interaction makes the equations of motion non-linear, it can modify the behaviour of the model very drastically. The most intriguing aspect of this behaviour is that the final properties of the perturbations become highly dependent on the initial values. Departures of Gaussian distribution are important observables of the primordial perturbations. Due to the non-linearity of the self-interacting curvaton model and its sensitivity to initial conditions, it can produce significant non-Gaussianity of the primordial perturbations. In this work we investigate the non-Gaussianity produced by the self-interacting curvaton, and demonstrate that the non-Gaussianity parameters do not obey the analytically derived approximate relations often cited in the literature. Furthermore we also consider a self-interacting curvaton with a mass in the TeV-scale. Motivated by realistic particle physics models such as the Minimally Supersymmetric Standard Model, we demonstrate that a curvaton model within the mass range can be responsible for the observed perturbations if it can decay late enough.

Inflazio kosmikoaren Fisika: Unibertsoaren egituraren jatorri kuantikoa

[ES] Analizamos el modelo de inflación cósmica más sencilla, y cómo este, a la vez que soluciona los problemas del modelo cosmológico estándar, es capaz de explicar el origen de la estructura a gran escala del universo.