Introduction to Cosmology

The Cold Dark Matter Paradigm 221 2 0 2 4 6 2 – 10 log(k Mpc/Ωh^2 ) CMB superclusters log( δM/M) 2 clusters CDM power spectr ...

222 Dark Matter With a large-scale bias of푏=1 to a precision of about 10%, the훽error dominates, so that one obtains 훺m= 0. 25 ± ...

10 Cosmic Structures After the decoupling of matter and radiation described in Chapter 6, we followed the fate of the free-strea ...

224 Cosmic Structures in the last scattering. The angular scale subtended by progenitors corresponding to the largest cosmic str ...

Density Fluctuations 225 wherekis the wave vector in comoving coordinates. An arbitrary pattern of fluctua- tions can be describ ...

226 Cosmic Structures Turning to short wavelengths (scale about 10^12 kg or 10−^18 푀⊙), black holes provide another constraint. ...

Density Fluctuations 227 Linear Approximation. Much of the interesting physics of density fluctuations can be captured by a Newt ...

228 Cosmic Structures But this difference need not be the same in′. For instance, even if an observable behaves as a scalar und ...

Structure Formation 229 a 1 a 2 Inflation (No inflation) H -^1 ~t~a 1/n H–^1 Standard cosmology log (length) Ngal = In(aH/a 2 ) ...

230 Cosmic Structures Note that only baryonic matter experiences pressure forces. Recall that dark matter is pressureless, feeli ...

Structure Formation 231 exist nonlinear modes they are outside it (the Jeans wavelength is greater than the horizon). A mass sca ...

232 Cosmic Structures The distortion of the CMB spectrum due to the SZE can be used to detect inter- galactic clouds and to prov ...

Structure Formation 233 Problems The mean free path퓁of photons in homogeneous interstellar dust can be found from Equation (1.4 ...

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11 Dark Energy TheFriedmann–Lemaitre universewhich we met in Chapter 5 has become the gener- ally accepted description of the Un ...

236 Dark Energy If휌휆were even slightly larger, the repulsive force would cause the Universe to expand too fast so that there wou ...

The Cosmological Constant 237 Explaining simultaneously all these and still other data, all consistent with an infla- tionary co ...

238 Dark Energy 90 80 H (z )/(1 + z) (km/sec/Mpc) 70 60 50 01 z 2 Figure 11.2 Measurements of 퐻(푧)∕( 1 +푧)versus푧demonstrating t ...

Single Field Models 239 with itself. In Section 7.2 we have already discussed this situation in the context of single-field infl ...

240 Dark Energy could do both jobs. Then the inflaton field and quintessence would have to be matched at some time later than푡GU ...