Introduction to Cosmology

Temperature Anisotropies 181 A B Figure 8.2The observer A in the solar rest frame sees the CMB to have dipole anisotropy—the len ...

182 Cosmic Microwave Background high퓁must be included. Anisotropies on the largest angular scales corresponding to quadrupoles a ...

Temperature Anisotropies 183 Curvature and isocurvature fluctuations behave differently when they are super- horizon: isocurvatu ...

184 Cosmic Microwave Background The gravitational redshift and the time dilation both contribute to훿푇∕푇 0 by amounts which are l ...

Polarizationpolarization 185 anisotropies found correspond to temperature variations of 훿푇= 29 ± 1 휇K, or 훿푇∕푇= 1. 06 × 10 −^5. ...

186 Cosmic Microwave Background yʹ y x xʹ zʹ β θ φ z e– γʹ γʹ Figure 8.4The geometry used in the text for describing the polariz ...

Polarizationpolarization 187 transforms to훼−휙. Thus the orientation does not define a direction, it only refers the polarization ...

188 Cosmic Microwave Background where휃is the scattering angle. By symmetry, Thomson scattering can generate no circular polariza ...

Model Testing and Parameter Estimation 189 of a scalar field (E for electric) and the curl of a vector field (B for magnetic). T ...

190 Cosmic Microwave Background The authors of the currently best measurement then end up presenting ten different versions rath ...

Model Testing and Parameter Estimation 191 introduced in Equation 5.20. The results are in agreement with other determinations, ...

192 Cosmic Microwave Background 500 D TEl /l [ μK 2 ] 0.4 0.2 0.2 0.4 Planck 143 +^217 0 1000 1500 2000 2500 l Figure 8.5The t ...

Model Testing and Parameter Estimation 193 The South Pole-based BICEP2 telescope [8] has observed the presence of the pri- mordi ...

194 Cosmic Microwave Background 0.0 0.2 0.4 0.6 0.8 1.0 ΩM 0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 Ω λ Decelerating Accelerating No Big ...

Model Testing and Parameter Estimation 195 occurred when훺m푎−^3 =훺r푎−^4. Using the value of훺mfrom (8.50) and훺rfrom (8.54) would g ...

196 Cosmic Microwave Background 0.0 0.1 0.2 0.3 0.4 0.5 0.6 ΩM 2.0 1.5 1.0 0.5 W Figure 8.7The 1휎and 2휎cosmological constraint ...

Model Testing and Parameter Estimation 197 Use Wien’s constant, Equation (6.120) and the CMB temperature to determine the wavel ...

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9 Dark Matter The analysis of anisotropies in the cosmic microwave background have shown that the fraction훺c= 0 .263 of all the ...

200 Dark Matter 9.1 Virially Bound Systems The planets move around the Sun along their orbits with orbital velocities balanced b ...