A hydrodynamic simulation has been developed to reproduce the properties of galaxies in the universe, including the distribution of galaxies in clusters, the statistics of hydrogen on large scales, and the metal and hydrogen content on small scales. The simulation starts 12 million years after the Big Bang and traces 13 billion years of cosmic evolution with 12 billion resolution elements in a volume of (106.5 Mpc)^3. It produces a reasonable population of elliptical and spiral galaxies, reproduces the distribution of galaxies in clusters, and accurately models the metal and hydrogen content of galaxies on small scales. The simulation uses the AREPO code, which employs a moving unstructured Voronoi tessellation in combination with a finite volume approach. It also includes a detailed model of galaxy formation physics, including the formation of stars and supermassive black holes, and their effects on their environments. The simulation successfully reproduces a mix of galaxy morphologies, including blue spiral galaxies and red ellipticals, with a hydrogen and metal content in good agreement with observational data. It also predicts the large-scale distribution of neutral hydrogen and the radial distribution of satellite galaxies within galaxy clusters. The simulation demonstrates that the ΛCDM model can correctly describe the variety of observational data on small and large scales in our universe. It also predicts a strong, scale-dependent impact of baryonic effects on the dark matter distribution, which has significant implications for future precision probes of cosmology. The simulation also shows that baryonic processes can impact and modify the dark matter distribution, altering the matter power spectrum P(k). The simulation's results are in remarkable agreement with observational data, demonstrating the effectiveness of the simulation in capturing the complex interplay of processes in galaxy formation. The simulation also shows that the impact of baryons on dark matter is significant and must be considered for future cosmological surveys. The simulation has also been used to create mock observations that mimic the conditions of the Hubble Space Telescope, providing benchmarks for galaxy formation theories. The simulation has also been used to study the internal characteristics of galaxies, including the stellar and gaseous contents of galaxies, and the baryonic cycle operating between them. The simulation has also been used to study the metallicity of galaxies and the distribution of neutral hydrogen in the intergalactic medium. The simulation has also been used to study the impact of baryons on the dark matter distribution and the matter power spectrum. The simulation has also been used to study the formation of low-mass galaxies and the challenges in modeling their formation. The simulation has also been used to study the impact of baryonic processes on the dark matter distribution and the matter power spectrum. The simulation has also been used to study the impact of baryonic processes on the dark matter distribution and the matter power spectrum. The simulation has also been used to study the impact of baryonic processes on the dark matter distribution and the matter power spectrum. The simulation has also been usedA hydrodynamic simulation has been developed to reproduce the properties of galaxies in the universe, including the distribution of galaxies in clusters, the statistics of hydrogen on large scales, and the metal and hydrogen content on small scales. The simulation starts 12 million years after the Big Bang and traces 13 billion years of cosmic evolution with 12 billion resolution elements in a volume of (106.5 Mpc)^3. It produces a reasonable population of elliptical and spiral galaxies, reproduces the distribution of galaxies in clusters, and accurately models the metal and hydrogen content of galaxies on small scales. The simulation uses the AREPO code, which employs a moving unstructured Voronoi tessellation in combination with a finite volume approach. It also includes a detailed model of galaxy formation physics, including the formation of stars and supermassive black holes, and their effects on their environments. The simulation successfully reproduces a mix of galaxy morphologies, including blue spiral galaxies and red ellipticals, with a hydrogen and metal content in good agreement with observational data. It also predicts the large-scale distribution of neutral hydrogen and the radial distribution of satellite galaxies within galaxy clusters. The simulation demonstrates that the ΛCDM model can correctly describe the variety of observational data on small and large scales in our universe. It also predicts a strong, scale-dependent impact of baryonic effects on the dark matter distribution, which has significant implications for future precision probes of cosmology. The simulation also shows that baryonic processes can impact and modify the dark matter distribution, altering the matter power spectrum P(k). The simulation's results are in remarkable agreement with observational data, demonstrating the effectiveness of the simulation in capturing the complex interplay of processes in galaxy formation. The simulation also shows that the impact of baryons on dark matter is significant and must be considered for future cosmological surveys. The simulation has also been used to create mock observations that mimic the conditions of the Hubble Space Telescope, providing benchmarks for galaxy formation theories. The simulation has also been used to study the internal characteristics of galaxies, including the stellar and gaseous contents of galaxies, and the baryonic cycle operating between them. The simulation has also been used to study the metallicity of galaxies and the distribution of neutral hydrogen in the intergalactic medium. The simulation has also been used to study the impact of baryons on the dark matter distribution and the matter power spectrum. The simulation has also been used to study the formation of low-mass galaxies and the challenges in modeling their formation. The simulation has also been used to study the impact of baryonic processes on the dark matter distribution and the matter power spectrum. The simulation has also been used to study the impact of baryonic processes on the dark matter distribution and the matter power spectrum. The simulation has also been used to study the impact of baryonic processes on the dark matter distribution and the matter power spectrum. The simulation has also been used