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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

Global Properties and Formation Scenarios

Session 6

Introduction by M. Fall

assembly
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

feedback
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?)

star formation
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):
slide5
AGN
  • What causes the tight BH-bulge relations?
  • Is the influence BH→bulge or bulge→BH?
  • When were these connections established?
scaling relations
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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