MODERN COSMOLOGY
Cosmic background fluctuations 87 the heat that flows during a reversible change. If no heat flows during a reversible change, t ...
88 An introduction to the physics of cosmology In a famous piece of serendipity, the redshifted radiation from the last- scatter ...
Cosmic background fluctuations 89 Figure 2.19. Illustrating the physical mechanisms that cause CMB anisotropies. The shaded arc ...
90 An introduction to the physics of cosmology 2.8.3 The temperature power spectrum The statistical treatment of CMB fluctuation ...
Cosmic background fluctuations 91 Here, the Bessel function comes from the angular part of the Fourier transform: ∫ exp(ixcosφ)d ...
92 An introduction to the physics of cosmology Doppler source term.The effect here is just the Doppler effect from the scatterin ...
Cosmic background fluctuations 93 where DLS= 2 c ^1 m/^2 H 0 ( 1 +zLS)−^1 /^2 = 184 (h^2 )−^1 /^2 Mpc is the comoving horizon ...
94 An introduction to the physics of cosmology whereqˆis a unit vector that specifies direction on the sky. Since the spherical ...
Cosmic background fluctuations 95 clustering, in the limit of a selection function that goes to a delta function in radius: C"SW ...
96 An introduction to the physics of cosmology We therefore expect that all scale-invariant models will have similar CMB power s ...
Cosmic background fluctuations 97 There were thus strong grounds to expect that large-scale fluctuations would be present at abo ...
98 An introduction to the physics of cosmology Figure 2.20.For 10% baryons, the value ofnneeded to reconcile COBE and the cluste ...
Cosmic background fluctuations 99 Figure 2.21.The geometrical degeneracy in the CMB means that models with fixedmh^2 andbh^2 c ...
100 An introduction to the physics of cosmology The physical degree of freedom here can be thought of as the Hubble constant. Th ...
Cosmic background fluctuations 101 V(φ). As well as the characteristic energy density of inflation,V, this can be characterized ...
102 An introduction to the physics of cosmology From the discussion of the Sachs–Wolfe effect, we know that, on large scales, th ...
Cosmic background fluctuations 103 Figure 2.22. Angular power spectraT^2 (")= "("+ 1 )C"/ 2 πfor the CMB, plotted against angula ...
104 An introduction to the physics of cosmology n= 1. 01 ± 0. 09. The only parameter left undetermined by the CMB is the Hubble ...
References 105 Ballinger W E, Peacock J A and Heavens A F 1996Mon. Not. R. Astron. Soc. 282877 Bardeen J M, Bond J R, Kaiser N a ...
106 An introduction to the physics of cosmology Hamilton A J S, Kumar P, Lu E and Matthews A 1991Astrophys. J. 374 L1 Hanany Set ...
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