I will provide an overview of the current status of simulations of proto-clusters and how they evolve to the population of mature low-redshift clusters. In particular, I will critically discuss open issues related to: (a) the strong star formation in proto-clusters; (b) the low level of star formation in nearby BCGs; (c) the metal share in stars and ICM.
The identification of substructures within halos in cosmological hydrodynamical simulations is a fundamental step to identify the simulated counterparts of real objects, namely galaxies. For this reason, substructure finders play a crucial role in extracting relevant information from the simulation outputs. They are based on physically-motivated definitions of substructures, performing...
Galaxy superclusters are exciting laboratories for a number of interesting processes in galaxy and cluster formation and evolution. Using GadgetIO, we simulate a cosmological box implementing constrained initial conditions from the local universe far into the future, obtaining final collapse regions for a number of local structures. While these regions contain interesting information about the...
The evolution of galaxy clusters is highly influenced by the dynamics of the Intracluster Medium (ICM), which governs crucial aspects. This includes mixing, turbulence processes, and galaxy interactions within the cluster environment. Among the factors influencing the ICM dynamics, the impact of viscosity is still under debate. Understanding the effect of viscosity on the evolution of galaxy...
Galaxy clusters are the most massive gravitationally bound objects in the Universe. Their number density offers a sensitive probe for the growth rate of large scale structure and the underlying cosmology. A way to produce this type of analysis is relying on wide-field optical imaging and photometric surveys, since they are capable of providing both large cluster samples and weak gravitational...
The process of gas accreting from the cosmic web onto galaxies is a fundamental aspect of galaxy formation. Simulations provide the tools to directly trace gas flows over time and are therefore crucial to test models and assumptions about accretion modes and geometry, which can then be used to interpret observational results. Using the Magneticum Pathfinder simulation box 4 (uhr), I trace gas...
Tidal features in the outskirts of galaxies detected by low surface brightness observations provide a unique pathway to study their assembly history. The upcoming Vera C. Rubin Observatory will provide a vast number of galaxies exhibiting such features, while integral field unit observations enable the study of their stellar population properties. I employ the hydrodynamical cosmological...
Observations of interacting galaxies in a cluster environments indicate that the triggered star formation activity inside the tidal tails is extending far beyond what we would expect from mergers in the field. Allowing to probe the possible parameter space, isolated setups are posing as the ideal testing ground to investigate the details and consequences of such behavior, as well as for a...
In large-scale simulations, that also include spectral cosmic-ray physics, high-energy protons and electrons accelerated at the shocks of supernova remnants have to be described by a sub-grid model. Usually, the injected cosmic rays are represented by a simple power-law spectrum in momentum space. However, in the recent past several models for more realistic cosmic-ray spectra from supernova...
The next generation of supercomputers will use a heterogeneous design to achieve exaflop capabilities. While this heterogeneous design offers significantly larger computational power it also increases the complexity of such systems. This has a significant impact on simulation codes to be run on these machines. Since the focus in the past was mainly on the scalability of CPUs with the...
Central massive black holes (BHs) and their host galaxies are thought to co-evolve also due to the complex interaction that arises when the BHs accrete gas and release a large amount of energy back into the surrounding environment.
Important actors in this scenario are powerful jets, and the spin of the central black hole is thought to be a key physical parameter that determines their power...
We study different numerical implementations of distributing the feedback energy from a central SMBH to the surrounding gas. We have incorporated a new sub-resolution model for the switching between thermal and kinetic AGN feedback modes depending on the BH accretion rate. Test simulations are being performed with cases of only thermal feedback, only kinetic feedback, and the combined...
Galaxy evolution models typically rely on SMBH feedback to quench massive galaxies. Therefore, accurately modeling the growth of these objects in our simulations is essential. In this talk, I will present an analysis of the star formation in local galaxies across different cosmic web environments, namely voids, walls, filaments, and nodes.
Interpreted using a semi-analytic model, the...
In the metal-enriched interstellar medium, the abundance of molecular gas is primarily governed by the formation of H2 on dust grains, as well as its self-shielding and shielding by dust against photo-dissociation by the interstellar radiation field. The upcoming presentation intends to describe a sub-resolution model for forming molecular hydrogen in hydrodynamic simulation with dust...
In this talk, I will present the current status of the new cooling implementation in OpenGADGET3. Specifically, I will refer to the first step of this project: the creation of new cooling tables, whose values were obtained using the CLOUDY code.
Hydrodynamic Cosmological Simulations offer a unique perspective in studying various aspects of structure formation in the universe. In particular, they hold great value in quantifying statistical properties such as the composition and enrichment of the baryonic matter distribution in the knots and filaments of the cosmic web. While it is observationally challenging to extract information from...
In this talk, I will present the current status of the implementation of Meshless Finite Mass (MFM) in OpenGadget3, which I implement as an alternative to the already implemented modern SPH solver.
MFM has several advantages over other solvers, such as developing mixing instabilities and capturing the power spectrum of subsonic turbulence. Thus, it also improves the description of...
I'll give an update on the state of the Spectral Cosmic Ray model in OpenGadget3.
In the metal-enriched interstellar medium, the abundance of molecular gas is primarily governed by the formation of H2 on dust grains, as well as its self-shielding and shielding by dust against photo-dissociation by the interstellar radiation field. The upcoming presentation intends to describe a sub-resolution model for forming molecular hydrogen in hydrodynamic simulation with dust...
