観測天文学特別講義VII

Formation and evolution of the cosmic web

We will examine the evolution of the universe, from the near-uniform matter distribution implied by the cosmic microwave background to present-day galaxies, clusters of galaxies, and the cosmic web. We will start by calculating the dynamics of the homogeneous, expanding universe, then discuss simple models of spherical collapse leading up to the formation of the first stars, galaxies, and hierarchical growth of structure.We will discuss the influence of cooling, star formation, and supermassive black holes in shaping today's universe, and take a detailed look at the physics of clusters of galaxies, the most massive structures in the cosmos.

MIMA Search

授業計画

(1) The expanding Universe: Hubble law, redshift, equations for expansion of homogeneous universe (matter, radiation, and cosmological constant dominated cases), discovery of CMB, basics of the thermal history of the Universe (2) The inhomogeneous Universe: perturbation theory, model of spherical collapse, the cold dark matter paradigm, N-body simulations of large-scale structure formation and comparison to current distribution of galaxies in the cosmic web; clusters of galaxies, the bremsstrahlung mechanism and Sunyaev-Zeldovich effect, shock heating and virialization during cluster assembly (3) The dark Universe: observational evidence for the cold dark matter paradigm: galaxy rotation curves, velocity dispersion, X-ray and gravitational lensing masses of galaxy clusters, search for self-interacting dark matter in cluster mergers. Candidates and experiments to search for DM (MACHOs, WIMPs, sterile neutrinos) (4) The radiant Universe: radiative cooling, the first stars, galaxy formation, feedback from supernovae and supermassive black holes (quasar and mechanical mode), co-evolution of supermassive black holes and galaxy bulges, the cooling flow problem (5) The chemistry of the Universe:Big Bang nucleosynthesis, thermonuclear vs. core-collapse supernova explosion models, metallicity measurements from optical and X-ray spectra, how metals are transported from the stars into the IGM: physics of ram pressure stripping, galactic winds (6) The geometry of the Universe: Type Ia SNe as standard candles, self-similarity of clusters of galaxies, CMB fluctuations + SZ effect, evidence for the accelerated expansion of the Universe and dark energy (7) The early Universe and the fate of the Universe: Models for dark energy beyond cosmological constant and observational tests,testing GR with growth of structure measurements, the Big Rip, inflation and the search for primordial gravitational waves; final review.