PHYS08200605006 D.K. Hazra - Homi Bhabha National Institute

More documents

Recommendations

Info

CHAPTER 7. IMPRINTS OF PRIMORDIAL NON-GAUSSIANITY IN THE LY-ALPHA FOREST k min (Mpc −1 ) ¯n (Mpc −2 ) S/N ∆f NL ∆b 1 2×10 −3 2.2×10 −3 5 228.84 1.1×10 −2 1×10 −3 2.2×10 −3 5 161.81 7.7×10 −3 5×10 −4 2.2×10 −3 5 114.42 5.5×10 −3 8×10 −4 1.0×10 −3 5 272.95 1.5×10 −2 8×10 −4 2.2×10 −3 5 144.73 6.9×10 −3 8×10 −4 5.0×10 −3 5 91.65 3.5×10 −3 8×10 −4 2.2×10 −3 2 263.52 1.5×10 −2 8×10 −4 2.2×10 −3 3 182.83 9.5×10 −3 8×10 −4 2.2×10 −3 4 156.56 7.7×10 −3 Ideal case 5×10 −4 1 5 23.72 2.1×10 −4 Table 7.1: The bounds on (f NL ,b 1 ) obtained from a Fisher analysis for various combinations of(k min ,¯n,S/N). ∆f NL ∼ 23 in the equilateral limit. We tabulate our results for varying sky coverage [k −3 min = V/(2π)3 ], Poisson noise (∼ 1/¯n) and pixel noise (S/N) in Table 7.1. As expected we have tighter constraints on (f NL ,b 1 ) with increasing survey volume, ¯n and S/N. The values of the survey parameters chosen are reasonable and achievable by future Ly-α surveys. Exploiting the entire sky coverage of SDSS we find that one can obtain a bound onf NL ∼ 100 (in the equilateral configuration) for a survey with ¯n = 5×10 −3 Mpc −2 when the spectra are measured at5-σ level [149]. Our analysis has largely focussed on the equilateral configuration. However we find that the Cramer-Rao bound for f NL in the squeezed limit (k 3
7.3. CONCLUSIONS 7.3 Conclusions To conclude, we emphasize that it is possible to put stringent bounds on primordial non- Gaussianity from the measured 3D bi-spectrum of the Ly-α forest along multiple lines of sight and thereby constrain various inflationary scenarios. Our analytic predictions indicate that such studies with future Ly-α surveys may be useful while performing a joint analysis using other data sets involving the CMB or LSS. 133
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 23 and 24:
List of Figures 1.1 A schematic tim
Page 25 and 26:
Chapter 1 Introduction At a first g
Page 27 and 28:
2.725K. It is also found to be high
Page 29 and 30:
1.1. THE CONCORDANT, BACKGROUND COS
Page 31 and 32:
1.2. THE INFLATIONARY PARADIGM 1.2
Page 33 and 34:
1.2. THE INFLATIONARY PARADIGM log
Page 35 and 36:
1.2. THE INFLATIONARY PARADIGM wher
Page 37 and 38:
1.2. THE INFLATIONARY PARADIGM wher
Page 39 and 40:
1.2. THE INFLATIONARY PARADIGM The
Page 41 and 42:
1.2. THE INFLATIONARY PARADIGM yet
Page 43 and 44:
1.3. THE GENERATION AND IMPRINTS OF
Page 45 and 46:
1.5. THE FORMATION OF THE LARGE SCA
Page 47 and 48:
1.7. NOTATIONS AND CONVENTIONS resu
Page 49 and 50:
Chapter 2 Generation of localized f
Page 51 and 52:
2.1. THE INFLATIONARY MODELS OF INT
Page 53 and 54:
2.2. METHODOLOGY, DATASETS, AND PRI
Page 55 and 56:
2.2. METHODOLOGY, DATASETS, AND PRI
Page 57 and 58:
2.3. BOUNDS ON THE PARAMETERS 2.3 B
Page 59 and 60:
2.3. BOUNDS ON THE PARAMETERS Model
Page 61 and 62:
2.4. THE SCALAR AND THE CMB ANGULAR
Page 63 and 64:
2.4. THE SCALAR AND THE CMB ANGULAR
Page 65 and 66:
2.5. DISCUSSION by the canonical sc
Page 67 and 68:
Chapter 3 Non-local features in the
Page 69 and 70:
3.1. MODELS AND METHODOLOGY on the
Page 71 and 72:
3.1. MODELS AND METHODOLOGY values
Page 73 and 74:
3.2. RESULTS Datasets WMAP-7 WMAP-7
Page 75 and 76:
3.2. RESULTS 0.2 0.15 0.1 ∆ χ 2
Page 77 and 78:
3.2. RESULTS 7000 150 6000 100 50 l
Page 79 and 80:
3.3. DISCUSSION WMAP as well as the
Page 81 and 82:
Chapter 4 Bi-spectra associated wit
Page 83 and 84:
4.1. MODELS OF INTEREST AND POWER S
Page 85 and 86:
4.1. MODELS OF INTEREST AND POWER S
Page 87 and 88:
4.2. THE SCALAR BI-SPECTRUM IN THE
Page 89 and 90:
4.3. THE NUMERICAL COMPUTATION OF T
Page 91 and 92:
Page 93 and 94:
Page 95 and 96:
Page 97 and 98:
Page 99 and 100:
Page 101 and 102:
Page 103 and 104:
Page 105 and 106: 4.4. RESULTS IN THE EQUILATERAL LIM
Page 107 and 108: 4.4. RESULTS IN THE EQUILATERAL LIM
Page 109 and 110: Chapter 5 The scalar bi-spectrum du
Page 111 and 112: 5.1. BEHAVIOR OF BACKGROUND AND PER
Page 123 and 124: 5.2. THE CONTRIBUTIONS TO THE BI-SP
Page 129 and 130: 5.3. DISCUSSION significant during
Page 131 and 132: Chapter 6 Effects of primordial fea
Page 133 and 134: 6.1. MODELS AND COMPARISON WITH THE
Page 135 and 136: 6.2. FROM THE PRIMORDIAL SPECTRUM T
Page 137 and 138: 6.3. THE NUMERICAL METHODS: ESSENTI
Page 139 and 140: 6.4. RESULTS Model Quadratic Quadra
Page 141 and 142: 6.4. RESULTS 6e-09 Quadratic potent
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: 7.2. RESULTS 0.12 0.13 2e3 , 2.2e3
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.
show all

PHYS08200605006 D.K. Hazra - Homi Bhabha National Institute

Create successful ePaper yourself

Delete template?

Save as template?