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The first part of the book discusses the basic ideas that have shaped our current understanding of the Early Universe. The discovering of the Cosmic Microwave Background (CMB) radiation in the sixties and its subsequent interpretation, the numerous experiments that followed with the enumerable observation data they produced, and the recent all-sky data that was made available by the Wilkinson Microwave Anisotropy Probe (WMAP) satellite, had put the hot big bang model, its inflationary cosmological phase and the generation of large scale structure, on a firm observational footing. An introduction to the Physics of the Early Universe is presented in K. The basic features of the hot Big Bang Model are reviewed in the framework of the fundamental physics involved.
Short- comings of the standard scenario and open problems are discussed as well as the key ideas for their resolution. It was an old idea that the large scale structure of our Universe might have grown out of small initial fluctuations via gravitational instability. Now we know that matter density fluctuations can grow like the scale factor and then the rapid expansion of the universe during inflation generates the large scale structure of our Universe. Durrer’s review offers a systematic treatment of cosmological perturbation theory.
After the introduction of gauge invariant variables, the Einstein and conservation equations are written in terms of these variables. The generation of perturbations during inflation is studied. The importance of linear cosmological perturbation theory as a powerful tool to calculate CMB anisotropies and polarisation is explained. The linear anisotropies in the temperature of CMB radiation and its po- larization provide a clean picture of fluctuations in the universe after the big bang.
These fluctuations are connected to those present in the ultra-high- energy universe, and this makes the CMB anisotropies a powerful tool for constraining the fundamental physics that was responsible for the generation of structure. Late time effects also leave their mark, making the CMB tem- www.com VI Preface perature and polarization useful probes of dark energy and the astrophysics of reionization. Challinor’s contribution discusses the simple physics that processes primordial perturbations into the linear temperature and polariza- tion anisotropies. The role of the CMB in constraining cosmological param- eters is also described, and some of the highlights of the science extracted from recent observations and the implications of this for fundamental physics are reviewed.
It is of prime interest to look for possible systematic uncertainties in the observations and their interpretation and also for possible inconsistencies of the standard cosmological model with observational data. This is important because it might lead us to new physics. Deviations from the standard cos- mological model are strongly constrained at early times, at energies on the order of 1 MeV. However, cosmological evolution is much less constrained in the post-recombination universe where there is room for deviation from stan- dard Friedmann cosmology and where the more classical tests are relevant.
Sander’s contribution discusses three of these classical cosmological tests that are independent of the CMB: the angular size distance test, the lumi- nosity distance test and its application to observations of distant supernovae, and the incremental volume test as revealed by faint galaxy number counts. The second part of the book deals with the missing pieces in the cosmo- logical puzzle that the CMB anisotropies, the galaxies rotation curves and microlensing are suggesting: dark matter and dark energy. It also presents new ideas which come from particle physics and string theory which do not conflict with the standard model of the cosmological evolution but give new theoret- ical alternatives and offer a deeper understanding of the physics involved. Our current understanding of dark matter and dark energy is presented in the review by V.
The review first focusses on issues pertaining to dark matter including observational evidence for its existence. Then it moves to the discussion of dark energy. The significance of the cosmological con- stant problem in relation to dark energy is discussed and emphasis is placed upon dynamical dark energy models in which the equation of state is time dependent. These include Quintessence, Braneworld models, Chaplygin gas and Phantom energy.
Model independent methods to determine the cosmic equation of state are also discussed. The review ends with a brief discussion of the fate of the universe in dark energy models. The next contribution by A. Lukas provides an introduction into time- dependent phenomena in string theory and their possible applications to cosmology, mainly within the context of string low energy effective theories.
A major problem in extracting concrete predictions from string theory is its large vacuum degeneracy. For this reason M-theory (the largest theory that includes all the five string theories) at present, cannot provide a coherent picture of the early universe or make reliable predictions. In this contribu- tion particular emphasis is placed on the relation between string theory and inflation.