Halo Population Map
Large-scale spatial distribution tracing halo structure.
GCC Multimedia
Seeing The Universe in a Nutshell
A selected visual representation of how gravity, plasma, and turbulence shape the universe at all scales.
From filaments stretching across hundreds of megaparsecs to the amplification of primordial magnetic fields in galaxy clusters, through the life cycle of generations of stars, each numerical step of the simulation captures physical phenomena that cannot be directly observed in real time but that we can now photograph here.
All image rights are reserved. If you are interested in using any material, please contact the GCC group.
Interactive model
Cosmic Web
The cosmic web within a MASCLET simulation of 40 Mpc side. The velocity field lines are displayed, depicting the inflow of matter into denser regions such as filaments (blue) and clusters (red). In yellow, regions with a considerable star formation are displayed.
Featured Simulation
Assembly of a Central Galaxy
The hierarchical formation of a central galaxy as a result of the merger between smaller galaxies as time progresses.
Watch full simulationSimulation Gallery
Large-scale structure
Magnetic 3D Structure
Field morphology highlighting how magnetic fields are induced along the different cosmic early structures.
Galaxies
Jellyfish Galaxy
Development of turbulence in the tail of a jellyfish galaxy falling in a massive galaxy cluster at z = 0.5.
Assembly of a Central Galaxy
The hierarchical formation of a central galaxy as a result of the merger between smaller galaxies as time progresses.
Magnetic fields and turbulence
3D Magnetic Field Evolution
Time-resolved amplification and reorganization of the magnetic field component in a cluster.
Primordial Magnetic Seed
Weak primordial seed generated for the beginning of the simulation.
Magnetic 3D Structure
Field morphology highlighting how magnetic fields are induced along the different cosmic early structures.
Computational methods
Adaptive Mesh Refinement Levels
Scanner of the dynamic resolution strategy concentrating computation on physically active regions.
Generative Modeling of N-body Simulations
N-body simulation at z = 0 created entirely using the generative model "Conditional Wasserstein Generative Adversarial Network".
Scientific Posters from the GCC
Conference poster
Imprints of the Internal Dynamics of Galaxy Clusters on the Sunyaev-Zeldovich Effect
This poster was presented at the SEA Scientific Meeting in 2024 by Òscar Monllor-Berbegal.
Conference poster
Origin and Mechanisms of Magnetic Field Amplification in Galaxies and Galaxy Clusters
This poster was presented at the 2nd IAA-CSIC Severo Ochoa Advanced School on Galaxy Evolution in 2025 by Marco Molina Pradillo.
Conference poster
The signature of major mergers on the hydroistatic mass bias on galaxy clusters
This poster was presented at the 2nd IAA-CSIC Severo Ochoa Advanced School on Galaxy Evolution in 2025 by Isac Barranco Llorca.
Behind the simulation
Each visual compresses billions of years of evolution into seconds. What appears as smooth color gradients encodes density, temperature, magnetic intensity, or velocity fields, computed by solving coupled gravitational and magneto-hydrodynamic equations on supercomputers. These simulations help us connect theory with observations, test physical models, and design future surveys.
Collaborate or request media material
Are you a researcher, communicator, or journalist interested in GCC simulation assets? We can share high-resolution renders, contextual explanations, and collaboration pathways for outreach or scientific partnerships.