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Global Properties and Formation Scenarios

Global Properties and Formation Scenarios. Session 6. Introduction by M. Fall. Assembly. Merging vs accretion lumpy or smooth Hot vs cold accretion importance of shocks Hierarchy vs something else massive old E galaxies at high z Disk vs spheroid

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Global Properties and Formation Scenarios

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  1. Global Properties and Formation Scenarios Session 6 Introduction by M. Fall

  2. Assembly • Merging vs accretion lumpy or smooth • Hot vs cold accretion importance of shocks • Hierarchy vs something else massive old E galaxies at high z • Disk vs spheroid physics of morphology • Disk-halo conspiracy Vc(R) ~ constant

  3. Feedback • How important is it in the mass, energy, and metal budgets of galaxies? (more for low-M galaxies?) • Is it driven by stars, AGN, or something else? (stars for low-M galaxies, AGN for high-M galaxies?) • How does it couple to the ISM of galaxies? (dependence on opacity and small-scale, multi-phase structure of the ISM?) • How does it affect galaxy assembly? (regulation or just removal?)

  4. Star Formation • SFR = fn (mass of gas,.…, other variables?) • Burst vs quiescent: different modes of SF or just different rates? • Tightness of dMs/dt vs Mg (Schmidt-Kennicutt) relation • Similarity of star and star cluster formation in interacting and normal galaxies • What causes “downsizing” (more recent SF in low-M galaxies):

  5. AGN • What causes the tight BH-bulge relations? • Is the influence BH→bulge or bulge→BH? • When were these connections established?

  6. Scaling Relations • V-R-C-Z-L relations and projections • When were they established? • How do they evolve? (slowly z = 0→1?) • Ancestor/descendant problem (LBGs, sub-mm sources, etc) • Comparisons with models • Bimodality: critical feature or wrinkle? • Evolution in number, masses, sizes of galaxies

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