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Cosmological Simulations of Galaxy Formation
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Cosmological Simulations of Galaxy Formation
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Over the last decades, cosmological simulations of galaxy formation have been instrumental for advancing our understanding of structure and galaxy formation in the Universe. These simulations follow the non-linear evolution of galaxies modeling a variety of physical processes over an enormous range of scales. A better understanding of the physics relevant for shaping galaxies, improved numerical methods, and increased computing power have led to simulations that can reproduce a large number of observed galaxy properties. Modern simulations model dark matter, dark energy, and ordinary matter in an expanding space-time starting from well-defined initial conditions. The modeling of ordinary matter is most challenging due to the large array of physical processes affecting this matter component. Cosmological simulations have also proven useful to study alternative cosmological models and their impact on the galaxy population. This review presents a concise overview of the methodology of cosmological simulations of galaxy formation and their different applications.
Forward citations
Cited by 10 Pith papers
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Non-Equilibrium Relativistic Core Collapse of Self-Interacting Dark Matter Halos -- Limits On Seed Black Hole Mass
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Probing the fate of large primordial perturbations with exoplanets
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Direct shear $\times$ kSZ correlation: controlling baryons without modeling galaxies
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Outflows in super-Eddington quasars drive clumpy circumgalactic medium and extended H$\alpha$ nebulae at $z \gtrsim 6$
In z≈6 quasar simulations, super-Eddington black-hole growth clears escape channels, ejects cold clumps that raise neutral-hydrogen covering, and powers extended Hα nebulae that shrink when the quasar is obscured.
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mitigating the overcooling problem with sink-based bursty star formation in a high-z dwarf galaxy
Sink-based star formation drives clump-scale bursts that pre-clear gas via radiation, raise SN momentum, cut stellar mass by ~3× and raise LyC escape by ~10× relative to a gravo-thermo-turbulent Schmidt model in a 10^...
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Non-Equilibrium Ionisation in Photoionised Haloes: Implications for Shock Stability and Absorption-Line Signatures
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Secondary Dependence of Baryonic Effects on the Density Profile of Dark Matter Halos
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Forged by Feedback: Stellar Properties of Brightest Group Galaxies in Cosmological Simulations
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