Speaker
Description
Future photometric and spectroscopic surveys will reveal unprecedented details about faint galaxies in massive clusters, requiring high-resolution theoretical models. Full-physics hydrodynamical simulations accurately reproduce galaxy properties but are computationally expensive, particularly for resolving low-mass galaxies in dense environments. In this work, we present an emulator based on SAG, a semi-analytic model, calibrated with hydrodynamical simulations within The Three Hundred project at a resolution of $7680^3$ particles (7K). This emulator successfully reproduces the properties of cluster galaxies at 7K and extends its predictions to simulations of $15360^3$ particles (15K), reaching stellar masses as low as $10^6 M_\odot$ and apparent magnitudes as faint as $m_H = 31$ at $z = 1$. The inclusion of orphan galaxies in SAG improves agreement with hydrodynamical results, enabling the study of faint satellite populations beyond the reach of current hydrodynamical simulations. Building on this work, we extend our analysis to the study of dwarf galaxies at 15K resolution in The Three Hundred project. This research aims to understand the structural and dynamical evolution of dwarf galaxies in dense environments, evaluating their star formation histories, metallicities, and possible transitions to globular clusters. Given the extreme density and resolution capabilities of 15K-SAG, this approach provides a unique opportunity to explore the evolution of low-mass galaxies in clusters, offering key predictions for future observational studies such as EUCLID, 4MOST-CHANCES, WEAVE, and other deep cluster galaxy surveys.
| Would you be interested in presenting a poster if the conference is oversubcribed? | No |
|---|
