PHYS08200605006 D.K. Hazra - Homi Bhabha National Institute

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CHAPTER 6. EFFECTS OF PRIMORDIAL FEATURES ON THE FORMATION OF HALOS Quadratic potential with a step ln β 0 −0.5 −1 −1.5 −2 −2.5 ln β 0 −1 −2 −3 −4 −5 −6 −7 14.62 14.64 14.66 14.68 14.7 14.72 14.74 0 5 10 15 20 φ 0 α x 10 −4 −8 0 10 20 α x 10 −5 Figure 6.2: The one dimensional likelihood on the parameter φ 0 in the case of the quadratic potential with a step (on the left) and the two dimensional constraints on the parameters α and β in the cases of the quadratic potential with sinusoidal modulations (in the middle) and the axion monodromy model (on the right). Note that the location of the stepφ 0 is well constrained. The inner and the outer curves (in the figure in the middle and the one on the right) correspond to the 1-σ and the 2-σ confidence contours. highly localized mass scales. We have also plotted the marginalized two dimensional constraints on the parameters α and β for the cases of the two oscillatory potentials. It is noteworthy that the constraints are strikingly similar. In fact, the roughly triangular shape of the contours can also be understood. As the parameterβ decreases, the resulting oscillations in the potential and, therefore, in the inflationary perturbation spectrum turn more frequent, and the data constrains the amplitude α to a smaller region. In Figure 6.3, we have plotted the best fit scalar power spectrum for the quadratic potential with and without the step and the two oscillatory potentials. Further below, in Figure 6.4, we have plotted the matter power spectrum P M (k) evaluated today corresponding to the different inflationary power spectra in the previous figure. In the inset of the figure, we have highlighted the baryon acoustic oscillations and the halo power spectrum data from SDSS LRG DR7. We should add here that the theoretical best fit curves are unable to fit the data well afterk ∼ 0.1hMpc −1 due to the fact that we have not taken the non-linear effects into account in arriving at the matter power spectrum. 6.4.2 Effects of features in the number density and the formation rate of halos In this section, we shall discuss the effects of the features on the number density and the formation rates of halos in the different inflationary models of our interest. In order 116
6.4. RESULTS 6e-09 Quadratic potential Quadratic potential with a step Quadratic potential with sinusoidal modulation Axion monodromy model 3e-09 P S (k) 1e-09 1e-05 0.0001 0.001 0.01 0.1 1 kMpc −1 Figure 6.3: The scalar power spectra that arise in the four inflationary models of our interest. These spectra correspond to the best fit values for which we had plotted the evolution of the first two slow roll parameters earlier. Note that, we have worked with the same choice of colors to represent the results from the different models as in the Figure 6.1. We should emphasize that, while the step model leads to features that are localized, the potentials with oscillatory terms lead to modulations in the scalar power spectrum that extend over a wide range of scales. to highlight the effects purely due to the primordial features, we have frozen the values of the background cosmological parameters, viz. Ω b , Ω m , Ω Λ and H 0 , at the values arrived at upon comparing the smooth quadratic potential with the WMAP and SDSS data (cf. Table 6.2). But, we have made use of the best fit values for the potential parameters to compute the inflationary scalar power spectrum and from thereon the matter power spectrum and the number density of halos. In Figure 6.5, we have plotted the percentage of change in the formation rate of halos in the Press-Schechter formalism and the number density of halos in the Sheth-Tormen formalism for different models with respect to the quadratic potential. In the case of the model with the step, the change in the number density due to the step (corresponding to, say, its best fit value) occurs at very high mass halos (∼ 10 17 M ⊙ ) and hence lies outside our region of interest. Due to this reason, we have only presented the results in the case of the models with oscillatory terms in the 117
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Primordial features and non-Gaussia
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Declaration This thesis is a presen
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Acknowledgments According to a popu
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Abstract Currently, inflation is th
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ABSTRACT tensors prove to be small
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ABSTRACT the best fit values arrive
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Contents 1 Introduction 1 1.1 The c
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CONTENTS 6 Effects of primordial fe
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List of Figures 1.1 A schematic tim
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Chapter 1 Introduction At a first g
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2.725K. It is also found to be high
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1.1. THE CONCORDANT, BACKGROUND COS
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1.2. THE INFLATIONARY PARADIGM 1.2
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1.2. THE INFLATIONARY PARADIGM log
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1.2. THE INFLATIONARY PARADIGM wher
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1.2. THE INFLATIONARY PARADIGM wher
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1.2. THE INFLATIONARY PARADIGM The
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1.2. THE INFLATIONARY PARADIGM yet
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1.3. THE GENERATION AND IMPRINTS OF
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1.5. THE FORMATION OF THE LARGE SCA
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1.7. NOTATIONS AND CONVENTIONS resu
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Chapter 2 Generation of localized f
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2.1. THE INFLATIONARY MODELS OF INT
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2.2. METHODOLOGY, DATASETS, AND PRI
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2.2. METHODOLOGY, DATASETS, AND PRI
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2.3. BOUNDS ON THE PARAMETERS 2.3 B
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2.3. BOUNDS ON THE PARAMETERS Model
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2.4. THE SCALAR AND THE CMB ANGULAR
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2.4. THE SCALAR AND THE CMB ANGULAR
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2.5. DISCUSSION by the canonical sc
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Chapter 3 Non-local features in the
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3.1. MODELS AND METHODOLOGY on the
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3.1. MODELS AND METHODOLOGY values
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3.2. RESULTS Datasets WMAP-7 WMAP-7
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3.2. RESULTS 0.2 0.15 0.1 ∆ χ 2
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3.2. RESULTS 7000 150 6000 100 50 l
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3.3. DISCUSSION WMAP as well as the
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Chapter 4 Bi-spectra associated wit
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4.1. MODELS OF INTEREST AND POWER S
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4.1. MODELS OF INTEREST AND POWER S
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4.2. THE SCALAR BI-SPECTRUM IN THE
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Page 131 and 132: Chapter 6 Effects of primordial fea
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Page 135 and 136: 6.2. FROM THE PRIMORDIAL SPECTRUM T
Page 137 and 138: 6.3. THE NUMERICAL METHODS: ESSENTI
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Page 143 and 144: 6.4. RESULTS 30 4 20 Change in R Ch
Page 145 and 146: 6.5. DISCUSSION wherein one works w
Page 147 and 148: Chapter 7 Imprints of primordial no
Page 149 and 150: 7.1. FORMALISM and the LSS studies.
Page 151 and 152: 7.1. FORMALISM only mildly non-line
Page 153 and 154: 7.1. FORMALISM If the bi-spectrum c
Page 155 and 156: 7.2. RESULTS 0.12 0.13 2e3 , 2.2e3
Page 157 and 158: 7.3. CONCLUSIONS 7.3 Conclusions To
Page 159 and 160: Chapter 8 Summary and outlook In th
Page 161 and 162: 8.2. OUTLOOK factorily [69, 70]. Ra
Page 163 and 164: Bibliography [1] See,http://magnum.
Page 165 and 166: BIBLIOGRAPHY [27] See,http://cfht.h
Page 167 and 168: BIBLIOGRAPHY [55] F. Arroja, A. E.
Page 169 and 170: BIBLIOGRAPHY [77] R. K. Jain, P. Ch
Page 171 and 172: BIBLIOGRAPHY [103] R. Allahverdi, J
Page 173 and 174: BIBLIOGRAPHY [132] S. Sasaki, Publ.
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PHYS08200605006 D.K. Hazra - Homi Bhabha National Institute

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