We introduce a novel high-resolution cluster simulation designed to serve as the massive halo counterpart of the modern cosmological galaxy evolution framework. The zoom-in simulation targets a volume of 4. 1σ overdensity region, which is expected to evolve into a galaxy cluster with a virial mass of 5 M_⊙, comparable to that of the Virgo Cluster. The zoom-in volume extends out to 3. 5 virial radii from the central halo. The novelties of M_⊙ is effective for tracing the early assembly of massive galaxies as well as the formation of dwarf galaxies. The spatial resolution of 68, parsecs in the best-resolved regions in the adaptive-mesh-refinement approach is a powerful tool for studying the detailed kinematic structure of galaxies. The time interval between snapshots is also exceptionally short (i. e. , 15 Myr). This is ideal for monitoring changes in the physical properties of galaxies, particularly during their orbital motion within a larger halo. The simulation includes up-to-date feedback schemes for supernovae (SNe) and active galactic nuclei (AGNs). The chemical evolution is calculated for ten elements, along with dust calculation that includes the formation, size change, and destruction. To overcome the limitations of the Eulerian approach used for gas dynamics in this study, we employed Monte Carlo-based tracer particles in 10^ 14 are exemplified by its resolution. Its stellar mass resolution of 2 10^ 4 enabling a wide range of scientific investigations. The simulation has passed z=0. 8, covering well over half of its cosmic history. We released the early data with the expectation they will facilitate studies of the early evolution of galaxies and overdensities.
Han et al. (Thu,) studied this question.