This course introduces the theoretical underpinnings and the observational evidence for modern cosmology.
After you learn what evidence exists for the hot Big Bang model, you study the basics of relativistic cosmology. We then discuss the physical processes occurring in the early universe, such as inflation, Big Bang nucleosynthesis and recombination. Finally, you will study the origin of large-scale structure, and use this to interpret the observations of the Cosmic Microwave Background. During the exercise classes, you will apply the material covered in the lectures in more involved calculations.
This course covers the following topics:
Relativistic cosmology (Friedmann equation, distances, basic parameters)
Thermal history of the Universe
Inflation
Big Bang nucleosynthesis
Recombination
Basics of structure formation
Interpretation of the Cosmic Microwave Background
Outcome:
How galaxies and the large-scale structures in which they are embedded form is a fundamental question in extra-galactic astronomy. It is an area that has seen tremendous progress, but is still constantly challenged by ever-improving observational data. This course introduces you to this fascinating subject and the underlying physics, starting from how small density perturbations grow into dark matter haloes, to how baryons cool and form the galaxy population we observe today. It will cover the main theoretical treatment of perturbations, as well as how to interpret the main observational probes of large-scale structure.
Physical concepts are derived from basic principles where possible. The emphasis is on intuitive rather than mathematically rigorous derivations.
Topics that will be covered include:
Linear growth of density perturbations
Free streaming
Transfer functions and the matter power spectrum
Non-linear spherical collapse
Jeans smoothing
Radiation drag
Statistical cosmological principle
Clustering and biasing
Halo mass functions and Press-Schechter theory
Scaling laws and virial relations
Cosmic web
Redshift-space distortions
Radiative cooling and its importance
Angular momentum and its influence
Reionization
The Gunn-Peterson effect
The thermal history of the intergalactic medium
Feedback processes
Halo models, semi-empirical models, and simulations
