SPFCU13

UE Stars and galaxies

Unité d'enseignement (UE) de 6 crédits

^En UE enseignée en Anglais

Contenu

Chemical evolution in the Solar neighborhood - Chemical evolution of galaxies - Analytic approximation to the (spectro)photometric evolution of galaxies (and limitations!) II. Galaxy spectral energy distribution Lecture 3: How to interpret the observed light received from galaxies ? (3h) O - Light from stars (single and composite stellar population) - Emission and absorption lines (links to parameters) - Dust (loi d’atténuation, Dale, Calzetti, macrospocic views, links with observations - Deriving statistical functions Lecture 4 : Inventory of the interstellar medium (2h) P - the different phases of the interstellar medium - simple models of the interstellar medium Lecture 5 : Physics of the interstellar medium (6h) P - the energy budget, heating and cooling - nebular emission lines and absorption lines - dust absorption, scattering and emission III. Feedback mechanisms Lecture 6 : Feedbacks at small scales (2h) P - interstellar medium evolution with super novae and stellar feedback Lecture 7: Feedback at large scale(3h) O - Stellar feedback (winds and outflows from supernova) - AGN feedback (from the accretion disk around supermassive black holes) IV. Galaxy evolution Lecture 8: Disk galaxies and their secular evolution (3h) O - Formation of a stellar disk - Galaxy Kinematic: observations - Galaxy Kinematic: some applications - Dynamical evolution Lecture 9: Elliptical galaxies and quenching: a violent history (3h) O - Galaxy properties (morphology, kinematic, scaling relations, supermassive black hole) - Formation scenario and mergers V. High-redshift galaxies Lecture 10: Formation of the first galaxies and Reionization (3h) R - Present constrains on the Re-ionization epoch & galaxy formation scenarios. Sources of the reionization. - Theoretical considerations: Hierarchical formation and abundance of CDM halos. Mass profiles. Press-Schechter formalism. Characteristic properties of collapsing halos. Galaxy formation models. Halo mass function. First stars and first galaxies. Reionization process. - Observational approaches : Identification and characterization of primeval galaxies. Observational signatures & properties. Observational Techniques. - Present results … and open issues. Discussion. Perspectives Lecture 11 : the interstellar medium of the first galaxies (2h) P - evolution of the interstellar medium after reionization - physics of the interstellar medium before reionization Lecture 12: Galaxy Assembly and Evolution in DM structures, clustering (2h) R - The Large Scale Structure (LSS) traced by galaxies. Large samples of galaxies from cosmological surveys. - Cosmological simulations of Galaxy Formation - Large Scale Structure and clustering properties: Mapping the density field. 2P correlation function (3D & projected CF). Redshift-space distortions. Galaxy bias. 2PCF in the local universe. 2PCD in the distant universe & redshift evolution. Connecting Galaxies to DM halos (Halo model interpretation, HOD + results)

UE Stars and galaxies

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