MODERN COSMOLOGY

Physics of temperature fluctuations 227 guarantees the distribution cannot have any azimuthal directional dependence. (The azimu ...

228 The cosmic microwave background is damping of baryon fluctuations on scales belowLD, known as Silk damping or diffusion damp ...

Physics of polarization fluctuations 229 Figure 7.1.The temperature angular power spectrum for a cosmological model with mass de ...

230 The cosmic microwave background as well, although quite generically the polarization fluctuations are expected to be signifi ...

Physics of polarization fluctuations 231 orientation of polarization. Note that the transformation law in equation (7.15) is cha ...

232 The cosmic microwave background only monopole and dipole directional dependences as explained earlier; therefore, scattering ...

Physics of polarization fluctuations 233 be expanded in terms of tensor spherical harmonics which preserve the correct transform ...

234 The cosmic microwave background amplitude and orientation of the polarization, then the G harmonics describe the portion of ...

Acoustic oscillations 235 Figure 7.2. The G polarization power spectrum (full curve) and the cross-power TG between temperature ...

236 The cosmic microwave background respect to conformal time.)and+are the scalar metric perturbations in the Newtonian gauge; ...

Acoustic oscillations 237 perturbation from the baryon–photon fluid,bγ, is non-zero or zero asη→0. The former case is known as ...

238 The cosmic microwave background in models producing perturbations causally on scales smaller than the horizon. Defect models ...

Cosmological models and constraints 239 oscillates arounda. If the oscillation amplitude is much larger thana= 3 ρb/ 4 ργ, th ...

240 The cosmic microwave background
, the ratio of the total energy density to the critical densityρcr= 8 π/ 3 H^2. This param ...

Cosmological models and constraints 241 spectra are generally defined so thatnT=0 corresponds to scale invariant, in contrast to ...

242 The cosmic microwave background describing scalar perturbations determine the size of the Sachs–Wolfe effect and also magnit ...

Cosmological models and constraints 243 shifted parameters will, in linear perturbation theory, produce almost exactly the same ...

244 The cosmic microwave background the agreement between the predicted and observed large-scale structure power spectrum. Massi ...

Cosmological models and constraints 245 in equations (7.31) is only an approximate equality is the pixelization noise. Most curr ...

246 The cosmic microwave background always be true for some sufficiently small range of parameter values. Then the parameter spa ...