PHYS08200605006 D.K. Hazra - Homi Bhabha National Institute

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List of Figures 1.1 A schematic timeline of the universe . . . . . . . . . . . . . . . . . . . . . . . 4 1.2 Evolution of the physical wavelength and the Hubble radius during the inflationary and the radiation dominated epochs . . . . . . . . . . . . . . . . 9 1.3 The theoretical and the observed CMB (TT) angular power spectra . . . . . 17 2.1 The difference inχ 2 eff with and without the step, plotted as a function of the multipoles . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 36 2.2 Typical evolution of the first slow roll parameter ǫ 1 and the quantity η around a step in an inflationary potential . . . . . . . . . . . . . . . . . . . . 37 2.3 The scalar power spectra corresponding to the best fit values of the WMAP seven-year data for inflationary models with the step . . . . . . . . . . . . . 38 2.4 The CMBTT angular power spectra corresponding to the best fit values of the inflationary models for the WMAP seven-year data without and with the step . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 39 3.1 The difference in χ 2 eff between the axion monodromy model and the reference model, plotted as a function of the multipoles . . . . . . . . . . . . . . . 51 3.2 The scalar power spectrum corresponding to the best fit values of inflationary potentials containing oscillatory terms . . . . . . . . . . . . . . . . . . . . 52 3.3 The CMB TT angular power spectrum in inflationary models containing oscillatory terms in the potential . . . . . . . . . . . . . . . . . . . . . . . . . 53 4.1 The scalar power spectra in the different types of models that we consider . 62 4.2 The behavior of the different contributions to the bi-spectrum, plotted as a function of cut off parameterκ, for the case of the quadratic potential . . . . 75 4.3 The behavior of the different contributions to the bi-spectrum, plotted as a function of the upper limit of the integrals, for the case of the quadratic potential . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 76 xxiii
Page 1: Primordial features and non-Gaussia
Page 5: Declaration This thesis is a presen
Page 9 and 10: Acknowledgments According to a popu
Page 11 and 12: Abstract Currently, inflation is th
Page 13 and 14: ABSTRACT tensors prove to be small
Page 15 and 16: ABSTRACT the best fit values arrive
Page 17 and 18: Contents 1 Introduction 1 1.1 The c
Page 19: CONTENTS 6 Effects of primordial fe
Page 24 and 25: LIST OF FIGURES 4.4 The spectral de
Page 26 and 27: CHAPTER 1. INTRODUCTION together co
Page 28 and 29: CHAPTER 1. INTRODUCTION Figure 1.1:
Page 30 and 31: CHAPTER 1. INTRODUCTION the spatial
Page 32 and 33: CHAPTER 1. INTRODUCTION say, λ P =
Page 34 and 35: CHAPTER 1. INTRODUCTION with the sc
Page 36 and 37: CHAPTER 1. INTRODUCTION sourced by
Page 38 and 39: CHAPTER 1. INTRODUCTION where the q
Page 40 and 41: CHAPTER 1. INTRODUCTION arise in su
Page 42 and 43: CHAPTER 1. INTRODUCTION 1.3 The gen
Page 44 and 45: CHAPTER 1. INTRODUCTION roll inflat
Page 46 and 47: CHAPTER 1. INTRODUCTION 1.6 Theme a
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Page 50 and 51: CHAPTER 2. GENERATION OF LOCALIZED
Page 68 and 69: CHAPTER 3. NON-LOCAL FEATURES IN TH
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CHAPTER 3. NON-LOCAL FEATURES IN TH
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CHAPTER 4. BI-SPECTRA ASSOCIATED WI
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CHAPTER 5. THE SCALAR BI-SPECTRUM D
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CHAPTER 6. EFFECTS OF PRIMORDIAL FE
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CHAPTER 7. IMPRINTS OF PRIMORDIAL N
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CHAPTER 8. SUMMARY AND OUTLOOK cien
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CHAPTER 8. SUMMARY AND OUTLOOK 138
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BIBLIOGRAPHY Kinney, arXiv:0902.152
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BIBLIOGRAPHY [39] V. N. Lukash, Sov
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BIBLIOGRAPHY [64] R. Easther, R. Fl
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BIBLIOGRAPHY [92] M. Kawasaki, F. T
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BIBLIOGRAPHY [118] K. Kohri, D. H.
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BIBLIOGRAPHY [145] P. McDonald, Ast
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PHYS08200605006 D.K. Hazra - Homi Bhabha National Institute

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