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[23] The Planck collaboration, “The Scientific Programme of Planck”, (2006), [arXiv:astro-ph/0604069] [24] Ue-Li Pen, “Brief Note: Analytical Fit to the Luminosity Distance for Flat Cosmologies with a Cosmological Constant”, (1999), [arXiv:astro-ph/9904172] [25] Lecture by Michael Doran, “A Primer on Cosmology and the Cosmic Microwave Background”, www.cmbeasy.org [26] Michael Doran, Christian M. Müller, Gregor Schäfer et al., “Gauge Invariant Initial Conditions and Early Time Perturbations in Quintessence Universes”, (2003), [arXiv:astro-ph/0304212] [27] Hideo Kodama and Misao Sasaki, “Cosmological Perturbation Theory”, Progress of Theoretical Physics Supplement, 78, (1984) [28] Viatcheslav Mukhanov, “Physical Foundations of Cosmology”, Cambridge University Press, (2005) [29] Chung-Pei Ma, Edmund Bertschinger, “Cosmological Perturbation Theory in the Synchronous and Conformal Newtonian Gauges”, (1995), [arXiv:astro-ph/9506072] [30] Andrew Liddle and David Lyth, “The Cold Dark Matter Density Perturbation”, (1993), [arXiv:astro-ph/9303019v1] [31] Kandaswamy Subramanian, “The Physics of CMBR Anisotropies”, (2004), [arXiv:astro-ph/0411049] [32] Will J. Percival , Robert C. Nichol , Daniel J. Eisenstein et al. , “The Shape Of The SDSS DR5 Galaxy Power Spectrum”, (2006), [arXiv:astro-ph/0608636] [33] Wayne Hu and Naoshi Sugiyama, “Anisotropies in the Cosmic Microwave Background: An Analytic Approach”, (1995), The Astrophysical Journal, 444: 489-506 [34] Wayne Hu and Naoshi Sugiyama, “Toward understanding CMB anisotropies and their implications”, (1995), Phys. Rev., Vol. 51: Nr.6 [35] Wayne Hu and Naoshi Sugiyama, “Small Scale Cosmological Perturbations: An Analytic Approach”, (1996), [arXiv:astro-ph/9510117] [36] V. Springel, S. D. M. White, A. Jenkins, “Simulating the joint evolution of quasars, galaxies and their large-scale distribution”, (2005), [arXiv:astro-ph/0504097] [37] A. J. S. Hamilton, P. Kumar, Edward Lu and Alex Matthews, “Reconstructing the Primordial Spectrum of Fluctuations of the Universe from the Observed Nonlinear Clustering of Galaxies”, (1991), The Astrophysical Journal, 374: L1-L4 [38] J.A. Peacock and S.J. Dodds, “Nonlinear evolution of cosmological power spectra”, (1996), [arXiv:astroph/960303] [39] R.E. Smith, J.A.Peacock, A.Jenkins et al. “Stable clustering, the halo model and nonlinear cosmological power spectra”, (2002), [arXiv:astro-ph/0207664] [40] Will Percival, http://www.dsg.port.ac.uk/∼percivalw/ [41] S. Zaroubi, M. Viel, A. Nusser et al. , “The matter power spectrum at small scales: an estimate from the Lyα forest optical depth”, (2005), [arXiv:astro-ph/0509563] [42] Zhaoming Ma, “The nonlinear matter power spectrum”, (2006), [arXiv:astro-ph/0610213] [43] J. Diemand, Ben Moore and J. Stadel, “Earth-mass dark-matter haloes as the first structures in the early Universe”, (2005), [arXiv:astro-ph/0501589] [44] Max Tegmark, http://space.mit.edu/home/tegmark/sdss.html [45] Shinji Tsujikawa, “Introductory Review of Cosmic Inflation”, (2003), [arxiv:hep-th/0304257] [46] Andrew R. Liddle and David H. Lyth, “Cosmological Inflation and Large-Scale Structure”, (2000), Cambridge University Press [47] I. K. Baldry, K. Glazebrook, T. Budavari et al., “The SDSS u-band Galaxy Survey: Luminosity functions and evolution”, (2005), [arxiv:astro-ph/0501110] 60 Bibliography
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Page 1:
Structure Formation in the Universe
Page 5 and 6:
Contents 1 Introduction 5 2 Equival
Page 7:
1 Introduction At high energies the
Page 10 and 11:
1. Spacetime is endowed with a symm
Page 12 and 13: One can see, that the differentials
Page 14 and 15: 3.5 The Connection 3.5.1 Geometric
Page 16 and 17: 3.7 Torsion andCurvature The Torsio
Page 18 and 19: It is an important property that th
Page 20 and 21: One concludes that the space of con
Page 22 and 23: 4.4 ScalefactorandRedshift For simp
Page 24 and 25: 4.6 The FriedmannEquations Summing
Page 26 and 27: 4.7.1 Values ofthedensityparameters
Page 28 and 29: 4.8 Inflation Inflation, first intr
Page 30 and 31: 10 1 1e+12 1e+10 1e+08 1e+06 10000
Page 32 and 33: With this metric, the velocity pert
Page 34 and 35: 5.2 InitialConditions According to
Page 36 and 37: CDM density perturbation today. Unf
Page 38 and 39: 100000 10000 1000 100 10 1 Dgγ Dg
Page 40 and 41: 10000 1000 100 10 1 0.001 0.01 k/h
Page 42 and 43: timesteps 1e+09 1e+08 1e+07 1e+06 1
Page 44 and 45: Performing on the other hand a Four
Page 46 and 47: α(Ω b,Ω c)=0.8873 andβ(Ω b,
Page 49 and 50: 8 The search for a cutoff Now the q
Page 51 and 52: 8 The searchfor a cutoff 49 ∆ 2 (
Page 53 and 54: Figure8.4: Luminosityfunction ofgal
Page 55: λ0/m Inflation aRH Radiation domin
Page 59 and 60: Descriptions Acbar: Arcminute Cosmo
Page 61: Bibliography [1] Clifford M. Will,
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Master Thesis

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