Relevant bibliographies by topics / Cosmology: large-scale structure of Universe

Academic literature on the topic 'Cosmology: large-scale structure of Universe'

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Published: 10 December 2022
Last updated: 24 February 2023

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Journal articles on the topic "Cosmology: large-scale structure of Universe"

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Bahcall, N. A. "Large Scale Structure of the Universe." Symposium - International Astronomical Union 179 (1998): 317–28. http://dx.doi.org/10.1017/s0074180900128906.

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How is the universe organized on large scales? How did this structure evolve from the unknown initial conditions of a rather smooth early universe to the present time? The answers to these questions will shed light on the cosmology we live in, the amount, composition and distribution of matter in the universe, the initial spectrum of density fluctuations that gave rise to this structure, and the formation and evolution of galaxies, lusters of galaxies, and larger scale structures.To address these fundamental questions, large and accurate sky surveys are needed—in various wavelengths and to various depths. In this presentation I review current observational studies of large scale structure, present the constraints these observations place on cosmological models and on the amount of dark matter in the universe, and highlight some of the main unsolved problems in the field of large-scale structure that could be solved over the next decade with the aid of current and future surveys. I briefly discuss some of these surveys, including the Sloan Digital Sky Survey that will provide a complete imaging and spectroscopic survey of the high-latitude northern sky, with redshifts for the brightest ∼ 106 galaxies, 105 quasars, and 103.5 rich clusters of galaxies. The potentialities of the SDSS survey, as well as of cross-wavelength surveys, for resolving some of the unsolved problems in large-scale structure and cosmology are discussed.
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PANCHAPAKESAN, N., and SHIV K. SETHI. "INFLATIONARY COSMOLOGY AND LARGE SCALE STRUCTURE OF THE UNIVERSE." International Journal of Modern Physics A 07, no. 16 (June 30, 1992): 3769–80. http://dx.doi.org/10.1142/s0217751x92001678.

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Scale-invariant (flat) fluctuation spectra are the most generic outcomes of inflation. However, current observations of large scale structure require more fluctuation power on large scales than flat spectra give. One such observation concerns the existence of large cosmological bubbles on the scales ~ (20–50) Mpc in the galaxy distribution. We attempt an explanation of these structures based on an inflationary model containing two scalar fields. One of these fields undergoes a first order phase transition, owing to the evolution of the other. We study the distribution of bubbles formed during the phase trnasition and show that for a wide range of choice of the free parameters in our model, a few bubbles can survive and grow to become the bubble structures observed at present.
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Suto, Yasushi. "Simulations of Large-Scale Structure in the New Millennium." Symposium - International Astronomical Union 216 (2005): 105–19. http://dx.doi.org/10.1017/s0074180900196548.

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Simulations of large-scale structure in the universe have played a vital role in observational cosmology since the 1980's in particular. Their important role will definitely continue to be true in the 21st century; indeed the requirements for simulations in the precision cosmology era will become more progressively demanding as they are supposed to fill the missing link in an accurate and reliable manner between the “initial” condition at z=1000 revealed by WMAP and the galaxy/quasar distribution at z=0 − 6 surveyed by 2dF and SDSS. In this review, I will summarize what we have learned so far from the previous cosmological simulations, and discuss several remaining problems for the new millennium.
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ELLIS, GEORGE F. R. "COSMOLOGY AND LOCAL PHYSICS." International Journal of Modern Physics A 17, no. 20 (August 10, 2002): 2667–71. http://dx.doi.org/10.1142/s0217751x02011588.

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This article considers the two-way relationship between local physics and the large scale structure of the universe - in particular considering Olber's paradox, Mach's principle, and the various arrows of time. Thus the focus is various ways in which local physics is influenced by the universe itself.
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Futamase, Toshifumi. "Gravitational lensing in cosmology." International Journal of Modern Physics D 24, no. 05 (March 18, 2015): 1530011. http://dx.doi.org/10.1142/s0218271815300116.

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Gravitational lensing is a unique and direct probe of mass in the universe. It depends only on the law of gravity and does not depend on the dynamical state nor the composition of matter. Thus, it is used to study the distribution of the dark matter in the lensing object. Combined with the traditional observations such as optical and X-ray, it gives us useful informations of the structure formation in the universe. The lensing observables depend also on the global geometry as well as large scale structure of the universe. Therefore it is possible to withdraw useful constraints on the cosmological parameters once the distribution of lensing mass is accurately known. Since the first discovery of the lensing event by a galaxy in 1979, various kinds of lensing phenomena caused by star, galaxy, cluster of galaxies and large scale structure have been observed and are used to study mass distribution in various scales and cosmology. Thus, the gravitational lensing is now regarded as an indispensable research field in the observational cosmology. In this paper, we give an instructive introduction to gravitational lensing and its applications to cosmology.
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Ruffini, R., D. J. Song, and S. Taraglio. "The Neutrino Mass and the Cellular Large Scale Structure of the Universe." Symposium - International Astronomical Union 124 (1987): 719–22. http://dx.doi.org/10.1017/s0074180900159820.

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We show how within the theoretical framework of a Gamow cosmology with massive neutrinos, the observed correlation functions between galaxies and between clusters of galaxies, naturally lead to a “cellular” structure of the Universe. From the size of “elementary cells” we derive constraints on the value of the masses and chemical potentials of the cosmological “inos”. We outline a procedure to estimate the “effective” average mass density of the Universe. We predict also the angular size of the inhomogeneities to be expected in the cosmological black body radiation as remnants of this cellular structure. A possible relation of our model to a fractal structure is indicated.
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Okamura, Sadanori, Elaine Sadler, Francesco Bertola, Mark Birkinshaw, Françoise Combes, Roger L. Davies, Thanu Padmanabhan, and Rachel L. Webster. "DIVISION VIII: GALAXIES AND THE UNIVERSE." Proceedings of the International Astronomical Union 4, T27A (December 2008): 283–85. http://dx.doi.org/10.1017/s1743921308025702.

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Division VIII provides a focus for astronomers studying a wide range of problems related to galaxies and cosmology. Objects of the study include individual galaxies, groups and clusters of galaxies, large scale structure, comic microwave background radiation and the universe itself. Approaches are diverse from observational one to theoretical one including computer simulations.
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Masaki, Shogo, Takahiro Nishimichi, and Masahiro Takada. "Anisotropic separate universe simulations." Monthly Notices of the Royal Astronomical Society 496, no. 1 (June 5, 2020): 483–96. http://dx.doi.org/10.1093/mnras/staa1579.

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ABSTRACT The long-wavelength coherent overdensity and tidal force, which are not direct observables for a finite-volume survey, affect time evolution of cosmic structure formation and therefore clustering observables through the mode coupling. In this paper, we develop an ‘anisotropic’ separate universe (SU) simulation technique to simulate large-scale structure formation taking into account the effect of large-scale tidal force into the anisotropic expansion of local background. We modify the treepmN-body simulation code to implement the anisotropic SU simulations, and then study the ‘response’ function of matter power spectrum that describes how the matter power spectrum responds to the large-scale tidal effect as a function of wavenumber and redshift for a given global cosmology. We test and validate the SU simulation results from the comparison with the perturbation theory predictions and the results from high-resolution particle-mesh simulations. We find that the response function displays characteristic scale dependencies over the range of scales down to non-linear scales, up to k ≃ 6 h Mpc−1.
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Silk, Joseph. "Origin and evolution of the large-scale structure of the universe." Canadian Journal of Physics 68, no. 9 (September 1, 1990): 799–807. http://dx.doi.org/10.1139/p90-117.

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Ever since the epoch of the spontaneous breaking of grand unification symmetry between the nuclear and electromagnetic interactions, the universe has expanded under the imprint of a spectrum of density fluctuations that is generally considered to have originated in this phase transition. I will discuss various possibilities for the form of the primordial fluctuation spectrum, spanning the range of adiabatic fluctuations, isocurvature fluctuations, and cosmic strings. Growth of the seed fluctuations by gravitational instability generates the formation of large-scale structures, from the scale of galaxies to that of clusters and superclusters of galaxies. There are three areas of confrontation with observational cosmology that will be reviewed. The large-scale distribution of the galaxies, including the apparent voids, sheets and filaments, and the coherent peculiar velocity field on scales of several tens of megaparsecs, probe the primordial fluctuation spectrum on scales that are only mildly nonlinear. Even larger scales are probed by study of the anisotropy of the cosmic microwave background radiation, which provides a direct glimpse of the primordial fluctuations that existed about 106 years or so after the initial big bang singularity. Galaxy formation is the process by which the building blocks of the universe have formed, involving a complex interaction between hydrodynamical and dynamical processes in a collapsing gas cloud. Both by detection of forming galaxies in the most remote regions of the universe and by study of the fundamental morphological characteristics of galaxies, which provide a fossilized memory of their past, can one relate the origin of galaxies to the same primordial fluctuation spectrum that gave rise' to the large-scale structure of the universe.
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Smoot, G. F. "Of Cosmic Background Anisotropies." Symposium - International Astronomical Union 168 (1996): 31–44. http://dx.doi.org/10.1017/s007418090010991x.

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Observations of the Cosmic Microwave Background (CMB) Radiation have put the standard model of cosmology, the Big Bang, on firm footing and provide tests of various ideas of large scale structure formation. CMB observations now let us test the role of gravity and General Relativity in cosmology including the geometry, topology, and dynamics of the Universe. Foreground galactic emissions, dust thermal emission and emission from energetic electrons, provide a serious limit to observations. Nevertheless, observations may determine if the evolution of the Universe can be understood from fundamental physical principles.
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Dissertations / Theses on the topic "Cosmology: large-scale structure of Universe"

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Dupuy, Hélène. "Precision cosmology with the large-scale structure of the universe." Thesis, Paris 6, 2015. http://www.theses.fr/2015PA066245/document.

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Cette thèse fournit des résultats innovants de plusieurs types. Leur point commun est la quête de précision dans la description des phénomènes physiques à l'œuvre dans l'univers. D'abord, un modèle-jouet simulant la propagation de la lumière dans un espace-temps non homogène est présenté. Dans cette étude, nous avons opté pour la traditionnelle représentation de type Swiss cheese. Souvent utilisée dans la littérature, elle permet de travailler avec des solutions exactes de la relativité générale, qui n'altèrent pas la dynamique globale de l'univers tout en le rendant fortement non homogène. Nous avons illustré la façon dont les hypothèses de base, telles que le principe cosmologique, peuvent affecter les conclusions scientifiques, telles que l'estimation des paramètres cosmologiques à partir des diagrammes de Hubble. Ce travail a donné lieu à deux publications en 2013, une dans Physical Review D et une autre dans Physical Review Letter. Le résultat majeur proposé dans cette thèse est une nouvelle façon de décrire les neutrinos en cosmologie. L'idée est de décomposer les neutrinos en plusieurs fluides à un flot de manière à se débarrasser de la dispersion en vitesse dans chacun d'eux. Cela s'inscrit dans le cadre de l'étude de la formation des grandes structures de l'univers à l'aide de la théorie des perturbations cosmologiques dans les régimes non linéaire et/ou relativiste. Ce travail a donné lieu à trois publications dans JCAP, une en 2014 et deux en 2015
This thesis provides innovative results of different types. What they have in common is the quest for precision in the description of the physical phenomena at work in the universe. First, a toy model mimicking the propagation of light in an inhomogeneous spacetime has been presented. In this study, we chose a traditional Swiss-cheese representation. Often used in the litterature, such models offer the advantage of dealing with exact solutions of the Einstein equations, which do not affect the global dynamics of the universe while making it strongly inhomogeneous. We have exemplified how initial presumptions, such as the cosmological principle, can alter scientific conclusions, such as the estimation of cosmological parameters from Hubble diagrams. This work resulted in two publications in 2013, one in Physical Review D and another one in Physical Review Letter. The major result exposed in this thesis is the proposition of a new way of dealing with the neutrino component in cosmology. The idea is to decompose neutrinos into several single-flow fluids in order to get rid of velocity dispersion in each of them. The research field to which it belongs is the study of the formation of the large-scale structure of the universe thanks to cosmological perturbation theory in the relativistic and/or nonlinear regimes. This work resulted in three publications in JCAP, one in 2014 and two in 2015
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Mehta, Kushal Tushar. "Measuring the Universe with High-Precision Large-Scale Structure." Diss., The University of Arizona, 2014. http://hdl.handle.net/10150/325226.

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Baryon acoustic oscillations (BAOs) are used to obtain precision measurements of cosmological parameters from large-scale surveys. While robust against most systematics, there are certain theoretical uncertainties that can affect BAO and galaxy clustering measurements. In this thesis I use data from the Sloan Digital Sky Survey (SDSS) to measure cosmological parameters and use N-body and smoothed-particle hydrodynamic (SPH) simulations to measure the effect of theoretical uncertainties by using halo occupation distributions (HODs). I investigate the effect of galaxy bias on BAO measurements by creating mock galaxy catalogs from large N -body simulations at z = 1. I find that there is no additional shift in the acoustic scale (0.10% ± 0.10%) for the less biased HODs (b < 3) and a mild shift (0.79% ± 0.31%) for the highly biased HODs (b > 3). I present the methodology and implementation of the simple one-step reconstruction technique introduced by Eisenstein et al. (2007) to biased tracers in N-body simulation. Reconstruction reduces the errorbars on the acoustic scale measurement by a factor of 1.5 - 2, and removes any additional shift due to galaxy bias for all HODs (0.07% ± 0.15%). Padmanabhan et al. (2012) and Xu et al. (2012) use this reconstruction technique in the SDSS DR7 data to measure Dᵥ(z = 0.35)(rᶠⁱᵈs/rs) = 1356 ± 25 Mpc. Here I use this measurement in combination with measurements from the cosmic microwave background and the supernovae legacy survey to measure various cosmological parameters. I find the data consistent with the ΛCDM Universe with a flat geometry. In particular, I measure H₀ = 69.8 ± 1.2 km/s/Mpc, w = 0.97 ± 0.17, Ωk = -0.004 ± 0.005 in the ΛCDM, wCDM, and oCDM models respectively. Next, I measure the effect of large-scale (5 Mpc) halo environment density on the HOD by using an SPH simulation at z = 0, 0.35, 0.5, 0.75, 1.0. I do not find any significant dependence of the HOD on the halo environment density for different galaxy mass thresholds, red and blue galaxies, and at different redshifts. I use the MultiDark N-body simualtion to measure the possible effect of environment density on the galaxy correlation function ℰ(r). I find that environment density enhances ℰ(r) by ∽ 3% at scales of 1 – 20h⁻¹Mpc at z = 0 and up to ∽ 12% at 0.3h⁻¹Mpc and ∽ 8% at 1 - 4h⁻¹Mpc for z = 1.
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McGill, Colin Andrew. "The large-scale structure of the universe : some theoretical considerations." Thesis, University of Oxford, 1987. http://ora.ox.ac.uk/objects/uuid:967fd0f2-817e-48ae-b57c-c1fb0dd435fb.

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In this thesis, several theoretical concepts relating to the large-scale structure of the universe are presented. In particular, various aspects of the hierarchical scenario are investigated. The initial perturbation field and its early evolution are discussed in Chapter 3. Chapter 4 is concerned with two-point correlation functions for galaxies, clusters and super-clusters. In Chapter 5, some effects of using velocity as a distance measure are examined. In particular, it will be argued that caustics in redshift space are an almost inevitable feature of the hierarchical scenario. Chapter 6 concentrates on the possibity that quasar Ly-α absorption lines are redshift caustics.
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Ntelis, Pierros. "Probing Cosmology with the homogeneity scale of the universe through large scale structure surveys." Thesis, Sorbonne Paris Cité, 2017. http://www.theses.fr/2017USPCC200/document.

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Cette thèse présente ma contribution à la mesure de l’échelle d’homogénéité à l’aide de galaxies, avec l’interprétation cosmologique des résultats. En physique, tout modèle est constitué par un ensemble de principes. La plupart des modèles de cosmologie sont basés sur le principe cosmologique, qui indique que l’univers est statistiquement homogène et isotrope à grande échelle. Aujourd’hui, ce principe est considéré comme vrai car il est respecté par ces modèles cosmologiques qui décrivent avec précision les observations. Cependant, l’isotropie de l’univers est maintenant confirmée par de nombreuses expériences, mais ce n’est pas le cas pour l’homogénéité. Pour étudier l’homogénéité cosmique, nous proposons un postulat d’homogénéité cosmique. Depuis 1998, les mesures des distances cosmiques à l’aide de supernovae de type Ia, nous savons que l’univers est maintenant en phase d’expansion accélérée. Ce phénomène s’explique par l’ajout d’une composante énergétique inconnue, appelée énergie sombre. Puisque l’énergie noire est responsable de l’expansion de l’univers, nous pouvons étudier ce fluide mystérieux en mesurant le taux d’expansion de l’univers. L’échelle d’oscillation acoustique Baryon (BAO). En mesurant cette échelle à différents moments de la vie de notre univers, il est alors possible de mesurer le taux d'expansion de l’univers et donc de caractériser cette énergie sombre. Alternativement, nous pouvons utiliser l’échelle d’homogénéité pour étudier cette énergie sombre. L’étude l’échelle de l’homogénéité et l’échelle BAO réclament l’étude statistique du regroupement de la matière de l’univers à grandes échelles, supérieure à plusieurs dizaines de Megaparsecs. Les galaxies et les quasars sont formés dans les vastes surdensités de la matière et ils sont très lumineuses: ces sources tracent la distribution de la matière. En mesurant les spectres d’émission de ces sources en utilisant de larges études spectroscopiques, telles que BOSS et eBOSS, nous pouvons mesurer leurs positions. Il est possible de reconstruire la distribution de la matière en trois dimensions en volumes gigantesques. Nous pouvons ensuite extraire divers observables statistiques pour mesurer l’échelle BAO et l’échelle d’homogénéité de l’univers. En utilisant les catalogues de diffusion de données 12 de la version 12 de données, nous avons obtenu une précision sur l’échelle d’homogénéité réduite de 5 par rapport la mesure de WiggleZ. À grande échelle, l’univers est remarquablement bien décrit en ordre linéaire selon le modèle LCDM, le modèle standard de la cosmologie. En général, il n’est pas nécessaire de prendre en compte les effets non linéaires qui compliquent le modèle à petites échelles. D’autre part, à grande échelle, la mesure de nos observables devient très sensible aux effets systématiques. Ceci est particulièrement vrai pour l’analyse de l’homogénéité cosmique, qui nécessite une méthode d’observation. Afin d’étudier le principe d’homogénéité d’une manière indépendante du modèle, nous explorons une nouvelle façon d’inférer des distances en utilisant des horloges cosmiques et SuperNovae de type Ia. C'est la théorie la plus couramment utilisée dans le domaine des hypothèses astrophysiques
This thesis exposes my contribution to the measurement of homogeneity scale using galaxies, with the cosmological interpretation of results. In physics, any model is characterized by a set of principles. Most models in cosmology are based on the Cosmological Principle, which states that the universe is statistically homogeneous and isotropic on a large scales. Today, this principle is considered to be true since it is respected by those cosmological models that accurately describe the observations. However, while the isotropy of the universe is now confirmed by many experiments, it is not the case for the homogeneity. To study cosmic homogeneity, we propose to not only test a model but to test directly one of the postulates of modern cosmology. Since 1998 the measurements of cosmic distances using type Ia supernovae, we know that the universe is now in a phase of accelerated expansion. This phenomenon can be explained by the addition of an unknown energy component,which is called dark energy. Since dark energy is responsible for the expansion of the universe, we can study this mysterious fluid by measuring the rate of expansion of the universe. Nature does things well: the universe has imprinted in its matter distribution a standard ruler, the Baryon Acoustic Oscillation (BAO) scale. By measuring this scale at different times in the life of our universe, it is then possible to measure the rate of expansion of the universe and thus characterize this dark energy. Alternatively, we can use the homogeneity scale to study this dark energy. Studying the homogeneity and the BAO scale requires the statistical study of the matter distribution of the universe at large scales, superior to tens of Megaparsecs. Galaxies and quasars are formed in the vast overdensities of matter and they are very luminous: these sources trace the distribution of matter. By measuring the emission spectra of these sources using large spectroscopic surveys, such as BOSS and eBOSS, we can measure their positions. It is thus possible to reconstruct the distribution of matter in 3 dimensions in gigantic volumes. We can then extract various statistical observables to measure the BAO scale and the scale of homogeneity of the universe. Using Data Release 12 CMASS galaxy catalogs, we obtained precision on the homogeneity scale reduced by 5 times compared to WiggleZ measurement. At large scales, the universe is remarkably well described in linear order by the ΛCDM-model, the standard model of cosmology. In general, it is not necessary to take into account the nonlinear effects which complicate the model at small scales. On the other hand, at large scales, the measurement of our observables becomes very sensitive to the systematic effects. This is particularly true for the analysis of cosmic homogeneity, which requires an observational method so as not to bias the measurement In order to study the homogeneity principle in a model independent way, we explore a new way to infer distances using cosmic clocks and type Ia SuperNovae. This establishes the Cosmological Principle using only a small number of a priori assumption, i.e. the theory of General Relativity and astrophysical assumptions that are independent from Friedmann Universes and in extend the homogeneity assumption
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Hatton, Stephen John. "Probing the large-scale structure of the Universe with future galaxy redshift surveys." Thesis, Durham University, 1999. http://etheses.dur.ac.uk/4494/.

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Several projects are currently underway to obtain large galaxy redshift surveys over the course of the next decade. The aim of this thesis is to study how well the resultant three-dimensional maps of the galaxy distribution will be able to constrain the various parameters of the standard Big Bang cosmology. The work is driven by the need to deal with data of far better quality than has previously been available. Systematic biases in the treatment of existing datasets have been dwarfed by random errors due to the small size of the sample, but this will not be the case with the wealth of data that will shortly become available. We employ a set of high-resolution /V-body simulations spanning a range of cosmologies and galaxy biasing schemes. We use the power spectrum of the galaxy density field, measured using the fast Fourier transform process, to develop models and statistics for extracting cosmological information. In particular, we examine the distortion of the power spectrum by galaxy peculiar velocities when measurements are made in redshift space. Mock galaxy catalogues are drawn from these simulations, mimicking the geometries and selection functions of the large surveys we wish to model. Applying the same models to the mock catalogues is not a trivial task, as geometrical effects distort the power spectrum, and measurement errors are determined by the survey volume. We develop methods for assessing these effects and present an in-depth analysis of the likely confidence intervals we will obtain from the surveys on the parameters that determine the power spectrum. Real galaxy catalogues are prone to additional biases that must be assessed and removed. One of these is the effect of extinction by dust in the Milky Way, which imprints its own angular clustering signal on the measured power spectrum. We investigate the strength of this effect for the SDSS survey.
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Melia, Fulvio. "The linear growth of structure in the Rh = ct universe." OXFORD UNIV PRESS, 2017. http://hdl.handle.net/10150/622916.

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We use recently published redshift space distortion measurements of the cosmological growth rate, f sigma(8)(z), to examine whether the linear evolution of perturbations in the R-h = ct cosmology is consistent with the observed development of large-scale structure. We find that these observations favour R-h = ct over the version of Lambda cold dark matter (Lambda CDM) optimized with the joint analysis of Planck and linear growth rate data, particularly in the redshift range 0 < z < 1, where a significant curvature in the functional form of f sigma(8)(z) predicted by the standard model-but not by R-h = ct-is absent in the data. When Lambda CDM is optimized using solely the growth rate measurements; however, the two models fit the observations equally well though, in this case, the low-redshift measurements find a lower value for the fluctuation amplitude than is expected in Planck Lambda CDM. Our results strongly affirm the need for more precise measurements of f sigma(8)(z) at all redshifts, but especially at z < 1.
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Manti, Serena. "Cosmic large scale structure: insights from radio astronomical experiments." Doctoral thesis, Scuola Normale Superiore, 2016. http://hdl.handle.net/11384/85877.

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From the introduction: "In this Thesis work we focus on the fundamental role that the Square Kilometre Array (SKA) will play in the search for Radio Recombination Lines (RRLs) from quasars and in radio-continuum observations of large scale structures, as, e.g. galaxy clusters. Moreover, we investigate the relationship between quasars and their host galaxies through studies of the cosmic LSS".
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Croft, Rupert Alfred Charles. "Galaxy clusters and the formation of large-scale structures in the universe." Thesis, University of Oxford, 1995. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.308751.

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Hoyle, Fiona. "The structure and scale of the universe." Thesis, Durham University, 2000. http://etheses.dur.ac.uk/4250/.

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We quantify the structure and scale of the Universe using redshift surveys of galaxies and QSOs and observations of Galactic open star clusters. We obtain the galaxy power spectrum from the Durham/UKST Galaxy Redshift Survey. By comparing the shape of the observed power spectrum to the APM real space power spectrum, we quantify the size of the redshift space distortions and find β = Ω(^0.6)/b=0.60±0.35. We also apply counts-in-cells analysis to the Durham/UKST and Stromlo-APM Surveys and measure the skewness directly out to 20h(^-1)Mpc. We find that the skewness measured from CDM models can only be reconciled with that of galaxies if bias is non-linear. We make predictions for the clustering in the 2dF QSO Survey by constructing mock catalogues from the Hubble Volume N-body simulation, with geometry, selection function and clustering matching those expected in the completed Survey. We predict that the correlation function will be reliably measured out to ~ 1, 000h(^-1)Mpc and the power spectrum out to 500h(^-1)Mpc. We measure the power spectrum from the 2dF QSOs observed by January 2000 and find it has a shape of F ~ 0.1. We also find little evolution in the clustering amplitude as a function of redshift. We obtain constraints on the cosmo- logical parameters Ωn and β by combining results from modeling geometric distortions introduced into the clustering pattern due to inconsistent cosmological assumptions and results from the QSO-mass bias. Finally, we consider the scale of the Universe. We check the calibration of the Cepheid Period-Luminosity relation using U,B,V and K'band imaging of Galactic Open Clusters containing Cepheids and measure the distance modulus to the LMC to be 18.51 ±0.10. However, we find anomalous colour-colour diagrams for two clusters and suggest that the effects of metallicity may be greater than previously considered.
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Collis, Olivari Lucas. "Intensity mapping : a new approach to probe the large-scale structure of the Universe." Thesis, University of Manchester, 2018. https://www.research.manchester.ac.uk/portal/en/theses/intensity-mapping-a-new-approach-to-probe-the-largescale-structure-of-the-universe(cd5b7586-7210-441e-838f-545d397893e5).html.

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Intensity mapping (IM) is a new observational technique to survey the large-scale structure of matter using emission lines, such as the 21 cm emission line of atomic hydrogen (HI) and the rotational lines of the carbon monoxide molecule (CO). Sensitive radio surveys have the potential to detect the HI power spectrum at low redshifts (z <1) in order to constrain the properties of dark energy and massive neutrinos. Observations of the HI signal will be contaminated by instrumental noise and, more significantly, by astrophysical foregrounds, such as the Galactic synchrotron emission, which is at least four orders of magnitude brighter than the HI signal. In this thesis, we study the ability of the Generalized Needlet Internal Linear Combination (GNILC) method to subtract radio foregrounds and to recover the cosmological HI signal for HI IM experiments. The GNILC method is a new technique that uses both frequency and spatial information to separate the components of the observed data. For simulated radio observations including HI emission, Galactic synchrotron, Galactic free-free, extragalactic point sources and thermal noise, we find that it can reconstruct the HI plus noise power spectrum with 7.0% accuracy for 0.13 <z <0.48 (960 - 1260 MHz) and l <400. In this work, GNILC is also applied to a particular CO IM experiment: the CO Mapping Array Pathfinder (COMAP). In this case, the simulated radio observations include CO emission, Galactic synchrotron, Galactic free-free, Galactic anomalous microwave emission, extragalactic point sources and thermal noise. We find that GNILC can reconstruct the CO plus noise power spectra with 7.3% accuracy for COMAP phase 1 (l <1800) and 6.3% for phase 2 (l <3000). In both cases, we have 2.4 <z <3.4 (26 - 34 GHz). In this work, we also forecast the uncertainties on cosmological parameters for the upcoming HI IM experiments BINGO (BAO from Integrated Neutral Gas Observations) and SKA (Square Kilometre Array) phase-1 dish array operating in auto-correlation mode. For the optimal case of BINGO with no foregrounds, the combination of the HI angular power spectra with Planck results allows w to be measured with a precision of 4%, while the combination of the BAO acoustic scale with Planck gives a precision of 7%. We consider a number of potentially complicating effects, including foregrounds and redshift dependent bias, which increase the uncertainty on w but not dramatically; in all cases the final uncertainty is found to be less than 8% for BINGO. For the combination of SKA-MID in auto-correlation mode (total-power) with Planck, we find that, in ideal conditions, w can be measured with a precision of 4% for the redshift range 0.35 <z <3 (350 - 1050 MHz) and 2% for 0 <z <0.49 (950 - 1421 MHz). Extending the model to include the sum of neutrino masses yields a 95% upper limit of less than 0.30 eV for BINGO and less than 0.12 eV for SKA phase 1, competitive with the current best constraints in the case of BINGO and significantly better in the case of SKA.
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Books on the topic "Cosmology: large-scale structure of Universe"

1

Fairall, Anthony. Large-scale structures in the universe. Cape Town: University of Cape Town, Department of Communication, 1998.

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Large-scale structures in the universe. Chichester, West Sussex, England: Wiley, 1998.

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Liddle, Andrew R. Cosmological inflation and large-scale structure. Cambridge, U.K: Cambridge University Press, 2000.

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Lincei, Accademia nazionale dei, and Scuola normale superiore (Italy), eds. Development of large-scale structure in the universe. Cambridge: published for the Accademia Nazionale dei Lincei and the Scuola Normale Superiore by the Press Syndicate of the University of Cambridge, 1991.

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Ostriker, J. P. Development of large scale structure in the Universe. Cambridge: Cambridge University Press, 1992.

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1951-, Dekel Avishai, and Ostriker J. P, eds. Formation of structure in the universe. New York: Cambridge University Press, 1999.

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Carola, Seitter Waltraut, Duerbeck Hilmar W. 1948-, and Tacke M. 1958-, eds. Large-scale structures in the universe: Observational and analytical methods. Berlin: Springer-Verlag, 1988.

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Coles, Peter. Is the universe open or closed? Cambridge: Cambridge University Press, 1997.

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Colloquium on the Age of the Universe, Dark Matter, and Structure Formation (1997 Irvine, Calif.). Colloquium on the Age of the Universe, Dark Matter, and Structure Formation. Washington, D.C: National Academy of Sciences, 1998.

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M, Mezzetti, and European Physical Society. Astronomy and Astrophysics Division., eds. Large scale structure and motions in the universe: Proceedings of an international meeting held in Trieste, Italy, April 6-9, 1988. Dordrecht: Kluwer Academic Publishers, 1989.

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Book chapters on the topic "Cosmology: large-scale structure of Universe"

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Vittorio, Nicola. "The Large Scale Structure of the Universe." In Astronomy, Cosmology and Fundamental Physics, 159–80. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0965-6_10.

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Bouchet, François R., and Lars Hernquist. "Implementation of a Tree Code for Cosmology." In Large Scale Structures of the Universe, 563. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2995-1_116.

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Bahcall, Neta A. "Large-Scale Structure in the Universe: Spatial Distribution and Peculiar Velocities." In Observational Cosmology, 335–48. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3853-3_32.

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Gott, J. Richard. "The Sponge-Like Topology of Large Scale Structure in the Universe." In Observational Cosmology, 433–36. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3853-3_40.

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Ruffini, R., D. J. Song, and S. Taraglio. "The Neutrino Mass and the Cellular Large Scale Structure of the Universe." In Observational Cosmology, 719–22. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3853-3_84.

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Martínez, V. J. "The Large-Scale Structure in the Universe: From Power Laws to Acoustic Peaks." In Data Analysis in Cosmology, 269–89. Berlin, Heidelberg: Springer Berlin Heidelberg, 2008. http://dx.doi.org/10.1007/978-3-540-44767-2_10.

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Kates, Ronald E. "Nonlinear Evolution of Acoustic Waves in Dust Interacting with Dark Matter in Newtonian Cosmology: Biasing, Voids, and the Kadomtsev-Petviashvill Equation." In Large Scale Structures of the Universe, 596. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2995-1_147.

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Mohanty, Subhendra. "Perturbations of the FRW Universe and Formation of Large Scale Structures." In Astroparticle Physics and Cosmology, 49–89. Cham: Springer International Publishing, 2020. http://dx.doi.org/10.1007/978-3-030-56201-4_3.

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Combes, Françoise, Patrick Boissé, Alain Mazure, and Alain Blanchard. "The Universe on a Large Scale." In Galaxies and Cosmology, 315–59. Berlin, Heidelberg: Springer Berlin Heidelberg, 2002. http://dx.doi.org/10.1007/978-3-662-04849-8_12.

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Combes, Françoise, Patrick Boissé, Alain Mazure, and Alain Blanchard. "The Universe on a Large Scale." In Galaxies and Cosmology, 293–332. Berlin, Heidelberg: Springer Berlin Heidelberg, 1995. http://dx.doi.org/10.1007/978-3-662-03190-2_12.

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Conference papers on the topic "Cosmology: large-scale structure of Universe"

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Sánchez, Ariel. "Precision Cosmology from large-scale structure observations." In VIII International Workshop on the Dark Side of the Universe. Trieste, Italy: Sissa Medialab, 2013. http://dx.doi.org/10.22323/1.161.0061.

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Matsubara, T. "Cosmology with the Large-Scale Structure of the Universe." In Proceedings of the KMI Inauguration Conference. WORLD SCIENTIFIC, 2013. http://dx.doi.org/10.1142/9789814412322_0009.

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Rantsev-Kartinov, V. A. "Large Scale Self-Similar Skeletal Structure of the Universe." In 1st CRISIS IN COSMOLOGY CONFERENCE, CCC-1. AIP, 2006. http://dx.doi.org/10.1063/1.2189125.

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Fry, J. N. "Large scale structure: Interpretation." In Cosmology and particle physics. AIP, 2001. http://dx.doi.org/10.1063/1.1363521.

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Sheth, Ravi K., Mario Novello, and Santiago Perez. "Large Scale Structure and Galaxies." In COSMOLOGY AND GRAVITATION: XIII Brazilian School on Cosmology and Gravitation (XIII BSCG). AIP, 2009. http://dx.doi.org/10.1063/1.3151838.

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Müller, Volker, Stefan Gottlöber, Jan P. Mücket, and Joachim Wambsganss. "Large Scale Structure: Tracks and Traces." In 12th Potsdam Cosmology Workshop. WORLD SCIENTIFIC, 1998. http://dx.doi.org/10.1142/9789814528467.

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Frieman, Joshua A. "Probing large-scale structure with galaxy surveys." In Cosmology and particle physics. AIP, 2001. http://dx.doi.org/10.1063/1.1363520.

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Mücket, Jan P., Stefan Gottlöber, and Volker Müller. "LARGE SCALE STRUCTURE IN THE UNIVERSE." In Proceedings of the International Workshop. WORLD SCIENTIFIC, 1995. http://dx.doi.org/10.1142/9789814532464.

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Einasto, Jaan, Remo Ruffini, and Gregory Vereshchagin. "Large scale structure of the Universe." In THE SUN, THE STARS, THE UNIVERSE AND GENERAL RELATIVITY: International Conference in Honor of Ya.B. Zeldovich’s 95th Anniversary. AIP, 2010. http://dx.doi.org/10.1063/1.3382336.

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KAPLINGHAT, MANOJ. "LARGE SCALE STRUCTURE OF THE UNIVERSE." In Proceedings of the Theoretical Advanced Study Institute in Elementary Particle Physics. WORLD SCIENTIFIC, 2011. http://dx.doi.org/10.1142/9789814327183_0013.

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