Who We Are
The Computational Cosmology Group is made up of two professors from the Department of Astronomy and Astrophysics at the University of Valencia, their respective doctoral students, and postdoctoral researchers who join the group through projects. To know more about our members, visit the Members section.
Lines of Research
Galaxy Formation and Evolution
One of the central challenges in modern astrophysics is understanding how galaxies form and evolve over cosmic time. This process involves both large-scale gravitational effects and small-scale baryonic physics, such as gas cooling, star formation, and feedback from supernovae and AGNs. Additionally, the role of supermassive black holes in shaping galaxy properties remains an open question. The group investigates the environmental effects on galaxy evolution, as well as the formation of rare galaxy types like ultra-diffuse galaxies (UDGs) and tidal dwarf galaxies. Their goal is to generate statistically significant galaxy catalogs from cosmological simulations and compare their properties with observational data.
Cosmic Structure Identification
The cosmic web is composed of voids, filaments, sheets, and galaxy clusters, each playing a distinct role in structure formation and galaxy evolution. Cosmic filaments, which connect clusters and span vast distances, contain the majority of warm-hot intergalactic medium and serve as highways for matter flowing into denser regions. Identifying and characterizing these filaments is crucial for understanding mass assembly, gas accretion, and environmental effects on galaxies. On the other hand, representing about 95% of the Universe's volume, cosmic voids provide a pristine environment for studying galaxy formation and the evolution of LSS. Unlike dense regions, voids experience fewer astrophysical interactions, making them ideal for testing cosmological models. However, characterizing void galaxies and filaments observationally is challenging due to their low density and faint nature. Through high-resolution simulations, the group seeks to analyze the statistical properties of voids and filaments, the formation of galaxies within them, and the nature of gas accretion flows in these underdense and transitional regions.
Cosmological shock waves
Shock waves, generated during the hierarchical formation of cosmic structures, play a crucial role in energy redistribution and the thermalization of baryonic matter. These waves are responsible for converting gravitational energy into thermal energy and contribute to magnetic field amplification and cosmic ray acceleration. Despite their significance, detecting them observationally remains challenging, making numerical simulations essential for understanding their properties, distribution, and impact on galaxy clusters and the intergalactic medium.
Cosmological Magnetic Fields
Magnetic fields are an essential component of the intergalactic medium, but their origin and amplification mechanisms are still not fully understood. Observations indicate that galaxy clusters host magnetic fields of ~0.1–10 μG, yet the transition from primordial weak fields to their present-day strengths is unclear. The group investigates the role of turbulence-driven dynamos in amplifying these fields and aims to create high-resolution magnetohydrodynamic (MHD) simulations that can be directly compared with future radio observations from instruments like the Square Kilometer Array (SKA).
Turbulence in the ICM
Turbulence is a fundamental process influencing the dynamics and thermodynamics of galaxy clusters. It arises from a variety of mechanisms, including matter accretion, galaxy motions, and feedback from active galactic nuclei (AGNs). Understanding turbulence is key to addressing issues such as non-thermal pressure contributions, hydrostatic mass biases, and gas mixing processes. Future observational facilities will allow for better characterization of turbulent motions through techniques like the kinetic Sunyaev-Zel’dovich (kSZ) effect, but numerical simulations remain crucial for interpreting these data and predicting observational signatures.
Fundings
- The formation of galaxies in the Large Scale Structure: simulations, PID2022-138855NB-C33, Agencia Estatal de Investigación, 1-9-2022 to 30-8-2026: IPs: S. Planelles, V. Quilis
