## Modern CosmologyModern Cosmology begins with an introduction to the smooth, homogeneous universe described by a Friedman-Robertson-Walker metric, including careful treatments of dark energy, big bang nucleosynthesis, recombination, and dark matter. From this starting point, the reader is introduced to perturbations about an FRW universe: their evolution with the Einstein-Boltzmann equations, their generation by primordial inflation, and their observational consequences. These consequences include the anisotropy spectrum of the cosmic microwave background (CMB) featuring acoustic peaks and polarization, the matter power spectrum with baryonic wiggles, and their detection via photometric galaxy surveys, redshift distortions, cluster abundances, and weak lensing. The book concludes with a long chapter on data analysis. Modern Cosmology is the first book to explain in detail the structure of the acoustic peaks in the CMB, the E/B decomposition in polarization which may allow for detection of primordial gravity waves, and the modern analysis techniques used on increasingly large cosmological data sets. Readers will gain the tools needed to work in cosmology and learn how modern observations are rapidly revolutionizing our picture of the universe. * Provides foundations, calculations, and interpretations which illuminate current thinking in cosmology * Covers the major advances in cosmology over the past decade * Includes over 100 unique, pedagogical figures |

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### Contents

The Standard Model and Beyond | 1 |

students in physics and astronomy and to advanced undergrads looking to get | 6 |

Exercises | 21 |

First many of the predictions are statistical We dont predict that there should | 27 |

Exercises | 53 |

Exercises | 80 |

The Boltzmann Equations | 84 |

is such a broad subject Many important papers discoveries and even subbranches | 97 |

Inhomogeneities | 180 |

Anisotropies | 216 |

Probes of Inhomogeneities | 261 |

Weak Lensing and Polarization | 292 |

Analysis | 336 |

A Solutions to Selected Problems | 392 |

B Numbers | 415 |

Symbols | 422 |

### Common terms and phrases

abundance amplitude angular anisotropy anisotropy spectrum baryon baryon density Big Bang Boltzmann equation Chapter Christoffel symbol comoving distance components Compton scattering compute coordinates correlation function cosmic cosmological constant covariance matrix critical density dark energy dark matter decoupling defined depends derivative deuterium dipole distribution function dominated early universe Einstein equations electrons energy density epoch equal equilibrium evolution Exercise expanding universe Figure first-order flat universe Fourier transform gauge Gaussian geodesic equation gravitational Hubble radius inflation integral last scattering likelihood function linear mass matter density matter-dominated measure metric modes momentum monopole multiply neutrinos neutron noise nonzero number density observations oscillator overdensity parameters particles photons pixel polarization potential power spectrum primordial quadrupole radiation ratio recombination redshift space scalar field scalar perturbations scale factor Section shows smaller solution spatial temperature tensor perturbations transfer function vanishes variables vector velocity wavelength window function zero zero-order