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Table of contents
1 Introduction
1.1 The epoch of reionization
1.1.1 A brief thermal history of the Universe
1.2 Observational constraints on reionization
1.2.1 Gunn-Peterson Troughs : Quasar absorption spectra
1.2.2 CMB polarization and temperature anisotropy
1.2.3 Other probes of reionization
1.3 21 cm line and reionization
1.3.1 The HI 21-cm probe
1.3.2 Brief review of numerical simulations of the EoR
1.4 Observing the 21 cm line
1.4.1 Tomography
1.4.2 Global signal
1.4.3 Power spectrum
1.4.4 Foreground Contamination
2 Numerical code – LICORICE
2.1 Tree SPH algorithm for dynamics
2.1.1 Tree algorithm for gravitation
2.1.2 The SPH algorithm for hydrodynamics
2.1.3 Additional physics
2.2 Monte Carlo on an adaptive grid – continuum
2.2.1 Adaptive grid
2.2.2 Ionizing radiation field
2.2.3 Absorption probability of photon packets
2.2.4 Updating physical quantities
2.2.5 Adaptive time integration
2.2.6 X-ray radiative transfer
2.3 Lyman line transfer
2.3.1 The optical depth
2.3.2 Hubble Expansion
2.3.3 Scattering off atoms
2.3.4 Propagation
2.3.5 Acceleration scheme
2.3.6 Further improvements for future
2.4 Radiative Transfer Comparison Test
2.4.1 Static density field cases
2.4.2 Radiative-hydrodynamics cases
2.5 Performance
3 The simulated 21 cm signal I
3.1 Physics of the 21 cm signal
3.1.1 Basic equations
3.1.2 The spin temperature
3.2 Lyman-alpha radiative transfer during the EoR
3.3 The simulated 21 cm signal during the EoR
4 The simulated 21 cm signal II
4.1 Source Model
4.1.1 Star Formation Rate
4.1.2 Luminosity and SED of the stellar sources
4.1.3 X-ray source model
4.2 Simulations
4.2.1 Initial condition
4.2.2 Global history of reionization
4.3 Helium reionization
4.4 QSO index
4.5 Luminosity of the QSO
4.6 The 21-cm signal
5 Galaxy formation with LICORICE
5.1 Initial conditions
5.2 Cooling rate and collisional equilibrium
5.3 Snapshot of the simulation
5.4 Discussion and prospects
6 Conclusion
A Cross-sections and rate coefficients
