Galaxy formation in cold dark matter
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1 Galaxy formation in cold dark matter Cheng Zhao Tsinghua Center for Astrophysics Oct 27, 2017 Main references: Press & Schechter, 1974 White & Rees, 1978
2 Galaxy formation mechanism Cosmological initial condition Gravitational instability Cosmic structure formation (dark haloes) Gas cooling Star formation galaxies
3 Galaxy formation mechanism Cosmological initial condition Gravitational instability Cosmic structure formation (dark haloes) Gas cooling Star formation galaxies
4 Cosmological initial condition Credit: APS/Alan Stonebraker
5 Galaxy formation mechanism Cosmological initial condition Gravitational instability Cosmic structure formation (dark haloes) Gas cooling Star formation galaxies
6 Gravitational instability Newtonian dynamics Scale: much smaller than the Hubble radius (light horizon)! L L h c/h Velocity: cold dark matter (non-relativistic)! v c Density: no highly relativistic objects at early Universe
7 Galaxy formation mechanism Cosmological initial condition Gravitational instability Cosmic structure formation (dark haloes) Gas cooling Star formation galaxies
8 Cosmic structure formation Two dimensionless parameters q = 4 3 m n G/h 2 Gravity vs. expansion of the Universe N J = n(v/h) 3 Gravity vs. pressure
9 Validation of self-similarity Macro-statistics q = 4 3 m n G/h 2 N J = n(v/h) 3 Dimensionless: two systems with the same q and NJ ought to condense similarly, regardless of the scale. Time evolution: possible self-similarity if q and NJ are constants in time.
10 Validation of self-similarity Micro-statistics Micro-statistical properties may differ, leading to different condensation mass function n(m) may rely on the initial condition different internal correlation Test on extreme cases Lower bound: particles are ordered in regular lattices. Upper bound: particles are statistically homogenous.
11 Spherical collapse model Spherical perturbation + collisionless dark matter Background expansion Gravitational collapse Credit: John D. Norton s web
12 Spherical collapse model Credit: Frank van den Bosch
13 Cosmic web structures Millennium-XXL simulation
14 Galaxy formation mechanism Cosmological initial condition Gravitational instability Cosmic structure formation (dark haloes) Gas cooling Star formation galaxies
15 Gas cooling Compton cooling (inverse Compton scattering with CMB photons at early Universe) Radiative cooling (rely on chemical composition, density, temperature ) Galaxy Formation & Evolution by H. Mo, F. van den Bosch & S. White
16 Gas cooling time scale t cool. H 1 Cooling vs. age of the Universe t cool. t dyn Cooling vs. pressure
17 Galaxy formation mechanism Cosmological initial condition Gravitational instability Cosmic structure formation (dark haloes) Gas cooling Star formation galaxies
18 Star formation Cold gas inflow Self-gravity dominates Fragment into stars
19 Galaxy formation mechanism Cosmological initial condition Gravitational instability Cosmic structure formation (dark haloes) Gas cooling Star formation galaxies
20 More Feedback Feedback mechanism for reheating Supernova feedback AGN feedback Rodrigues 2010
21 More Mergers Mergers of haloes: a bottom-up manner More massive galaxies have higher metallicity Formation of elliptical galaxies More satellites Star bursts Credit: Marta Volonteri
22 Unknowns Gas mass fraction Time scale of different mechanisms Initial mass function Feedback efficiency
23 Hydro-dynamical simulations Credit: EAGLE Project Consortium/Schaye+ 2014
24 Unresolved problems Core or cusp Walker & Loeb 2014
25 Unresolved problems Too big to fail Garrison-Kimmel+ 2014
26 Unresolved problems Missing satellite Weinberg+ 2015
27 Summary Structure formation in CDM cosmology. Gas cooling and collapse in dark haloes. Gas fragmentation and formation of stars/galaxies. Merger/feedback processes. Problems due to CDM or baryonic effects?
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