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Table of contents
Introduction
0.1 Structure formation in the early universe: linear perturbation theory
0.2 Spherical collapse and Press-Schechter theory
0.3 The cosmic web
0.4 Galactic morphologies
0.5 Structure of this Thesis
1 Numerical Methods
1.1 Simulating the universe on cosmological scales
1.1.1 RAMSES: basic features
1.1.2 Small-scale physical recipes for realistic galactic dynamics.
1.2 Structure detection and identification in Horizon-AGN
1.2.1 Haloes and galaxies: Structure identification and merging
1.2.2 Synthetic galaxies in Horizon-AGN
1.2.3 The numerical cosmic web
2 Galactic spin alignments induced by the cosmic web
2.1 Orientation of dark haloes in the cosmic web
2.1.1 The spin of dark haloes: a mass segregated distribution
2.1.2 Tidal Torque Theory
2.1.3 A dynamical scenario
2.1.4 Mergers versus smooth accretion
2.1.5 From haloes to galaxies
2.2 Tracing galactic spin swings in the cosmic web
2.2.1 Numerical Methods
2.2.2 Evolution tracers
2.2.3 Alignments in Horizon-AGN
2.2.4 Comparison to observations
2.3 How mergers drive spin swings in the cosmic web
2.3.1 Tracking mergers in Horizon-AGN
2.3.2 Mergers, stellar mass and spin in Horizon-AGN: close-up case studies
2.3.3 Mergers and smooth accretion on spin orientation
2.3.4 Mergers and smooth accretion on acquisition of spin.
2.4 Conclusion
3 Orientation of satellites galaxies: massive hosts versus the cosmic web
3.1 An overview of satellite galaxies
3.1.1 The formation of satellite galaxies in CDM cosmology
3.1.2 The distribution of satellite galaxies
3.2 Satellites in Horizon-AGN
3.2.1 Identifying central galaxies and satellites
3.2.2 Tracing the evolution of satellites in the halo: synthetic colors.
3.3 Statistical properties of the orientation of satellites
3.3.1 Methods and variables
3.3.2 Results
3.4 A dynamical scenario : satellites migrating into the halo.
3.4.1 Scenario
3.4.2 Corotation of satellites
3.4.3 Evolution of satellites within the halo
3.5 Implications for observations.
3.5.1 Color selection
3.5.2 Signal on smaller scales
3.5.3 Effects of the shape of the central host and high-z alignments.
3.6 Conclusion.
4 The rise and fall of stellar disks at z > 1
4.1 Inflows and galaxy encounters: an overview
4.1.1 Disc galaxies: evolution of the Hubble sequence with redshift
4.1.2 Violent Disc Instability: the path to compact spheroids
4.1.3 Mergers
4.1.4 Dry or wet mergers? Extended spheroids and massive disks.
4.2 Characterizing different types of mergers in Horizon-AGN
4.2.1 Characterizing the morphology of galaxies
4.2.2 Gas content of high-z galaxies
4.2.3 Merger rates: from observations to simulation
4.3 Size growth of galaxies
4.3.1 Galactic stellar density
4.3.2 Galactic half-mass radius
4.3.3 Impact of initial gas fraction and morphology
4.4 Impact on morphologies
4.4.1 Smooth accretion
4.4.2 Mergers
4.5 Conclusion
4.6 Main results
4.7 Prospects
4.7.1 Sorting out the merger zoo
4.7.2 Gas inflows: feeding galaxies into diverse morphologies ?
4.7.3 Distribution of satellites
Bibliography
