Title Page
Abstract
Contents
Chapter 1. Introduction 12
1.1. Brief Summary Of Modern Galaxy Formation Theory 13
1.2. Toward A Holistic Picture Of Baryon Processes In Galaxies 18
Chapter 2. Impact Of Baryon Physics On The Formation Of Dark Matter Deficient Galaxies 24
2.1. Introduction 24
2.2. Simulations 28
2.2.1. A Suite of Idealized Galaxy Collision Simulations 28
2.2.2. A Large Simulated Universe TNG100-1 32
2.3. Dark Matter Deficient Galaxies (DMDGs) Produced In High-velocity Galaxy Collision Simulations 34
2.3.1. Definition Of A Dark Matter Deficient Galaxy (DMDG) 34
2.3.2. Idealized Fiducial Simulation: High-velocity Collision Between Two Dwarf Galaxies 39
2.3.3. Parameter Study: In What Type of Galaxy Collision Can A DMDG Form? 45
2.4. Looking For High-velocity Galaxy Collision Events In A Large Simulated Universe 47
2.4.1. Number Of High-velocity Galaxy Collision Events In TNG100-1 That Could Have Produced DMDGs 47
2.4.2. Example: How Would A DMDG-producing Galaxy Collision Event Look Like? 49
2.4.3. Idealized Simulation: High-velocity Collision Between Two Satellite Galaxies Near A Massive Host 52
2.5. Looking For "Collision-induced" DMDGs in A Large Simulated Universe 54
2.5.1. Looking For Collision-induced DMDGs in the TNG100- 1 Halo Catalogues 54
2.5.2. Looking For Collision-induced DMDGs in the TNG100- 1 Simulation Snapshots 62
2.5.3. Difference Between High-resolution (80 pc) Simulations And The Large Cosmological Simulation: Importance Of Spatial Resolution 66
2.6. The Inner Structure Of Collision-induced Dark Matter-Deficient Galaxies 68
2.6.1. Idealized Galaxy Collision Simulations With 1.25 Resolution 68
2.6.2. Kinematics And Morphology Of Collision-induced Dark Matter Deficient Galaxies 70
2.6.3. Star Clusters In The Collision-Induced DMDGs: Formation History And Key Observables 76
2.7. Conclusion 77
Chapter 3. Impact Of Stellar Physics On The Baryon Cycle Within Galaxies 80
3.1. Introduction 80
3.2. Simulations 83
3.2.1. Initial Conditions 83
3.2.2. Simulation Setup 84
3.2.3. Suite Of Simulations 91
3.3. Spatial Distribution Of Gas And Stars 92
3.3.1. Spiral Arm Properties 92
3.3.2. Massive Clump Properties 94
3.3.3. Spatial Power Spectral Density (PSD) Of The Star Formation Rate (SFR) 94
3.4. How Gas Cycles Through The Galaxy And Forms Stars 98
3.4.1. Residence Time In Dense Versus Diffuse Regions 99
3.4.2. Tracking Individual Gas Parcels 101
3.4.3. Correlation Between Star Formation Variability And The Baryon Cycle 112
3.5. Discussion 116
3.5.1. Implications For The Baryon Cycle Within Galaxies 116
3.5.2. Observational Implications 118
3.5.3. Caveats Of The Analysis 119
3.6. Conclusion 120
Chapter 4. Impact Of Properties Of Hydrodynamic Solver On Metal Distribution Of Galaxies In Numerical Simulations 124
4.1. Introduction 124
4.2. Numerical Methods 130
4.2.1. Simulation Codes 130
4.2.2. Initial Condition 134
4.2.3. Baryon Physics 136
4.3. Metal Distribution In Halo: Dependence On Initial Gas Distribution And Feedback Strength 141
4.3.1. Comparison Of Star Formation Rates 144
4.3.2. Overview: Metal Distribution And Outflow Velocity 146
4.3.3. Spatial Profiles Of Metals And Its Evolution In Time 148
4.3.4. Metal Distribution In The Density-Temperature Plane 154
4.4. Metal Distribution In Halo: Dependence On Explicit Metal Diffusion Schemes 156
4.4.1. Metallicity Distribution Function 158
4.4.2. Pockets of Metal-poor Gas 162
4.5. Generalizing Our Findings In Another Particle-based Code 163
4.6. Conclusion 164
Chapter 5. Conclusion And Future Work 168
5.1. Conclusion 168
5.2. Future Work 172
Bibliography 176
Appendix 212
E.3. Effect Of Varying The Resolution 212
E.4. PSD Fitting 216
국문초록 218