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The ?eld of cosmology is currently undergoing a revolution driven by d- matic observational progress and by novel theoretical scenarios imported from particle physics. In particular, two most remarkable results were recently - tained from measurements of the angular spectrum of the ?uctuations in the Cosmic Microwave Background (CMB) radiation providing convincing e- dence that the Universe is nearly ?at and from the Hubble diagram of distant supernovae indicating an accelerating expansion rate, which implies the ex- tence of some dark energy as the dominant component of the Universe. Indeed, the next decade will bene?t from high quality data on cosmology from diff- ent major experiments and observatories, with a particular important contri- tion from space missions such as WMAP, Planck Surveyor, XMM and SNAP among others. On one side, cosmologists believe they understand the origin of themain ingredients which allowacoherent description of theUniverse from its very earlyphase, namely in?ation, to the actual epoch which accounts for theoriginof theprimordial?uctuations, allowing predictions of their - prints inthe cosmicmicrowave skyandleading to the large scale structure of theUniverse as observed. Ontheother side, theexistence of a non-zero vacuum density is certainly one of the most astonishing results of modern f- damental physics. Understanding its nature andits originwill be one of the major directions of researchinthe following years. In view of the intensive current activity inthe ?eld,aSchoolfully dedicated to these both sides in cosmology was timely.
Inhalt
Dedication, Preface Acknowledgments;
1 Basics of Cosmology
Geometry and Dynamics ; 2.Important quantities needed for observations
Some solutions of EFL equations:some cosmological models; 4. The standard Big Bang Nucleosynthesis (SBBN);5. Observations of primordial abundances'; 6. Confrontation of the observed
primordial abundances'' to the predictions of the sBBN; Conclusions; References
2 X-ray View of Galaxy Clusters,
3 Clusters: an optical point of view;
4 Cosmology with Clusters;
Introduction;2. What is a cluster? ; 3. The spherical model;4. The mass function;
Connection to the observations; 6. Properties of Clusters and scaling relations; 7. Clusters abundance evolution; 8. The baryon fraction; 9. Conclusion; References
5 Astrophysical detection of Dark Matter ;
6 Non-thermal processes in galaxy clusters ;
7 Cosmological Inflation ;
8 An introduction to quintessence ;
9 CMB Observational Techniques and Recent Results
10 Fluctuations in the CMB ; Andrew H. Jaffe
11 Supernovae as astrophysical objects;
Some History;2. Supernova classification;3. Input Energy;4. Core-collapse supernovae ;
Type Ia supernovae ;6. Conclusions; References
12 Cosmology with Supernovae ;
13 Gravitational lensing;
14 Dark Matter ;
Introduction;2. Local Dark Matter;3. Clusters and Groups of Galaxies;4. Masses of Galaxies ;
The Nature of Dark Matter;6. Summary;Acknowledgments;References
15 Dark Matter and Galaxy Formation;
16 Non-Baryonic Dark Matter;