We aim at modeling galaxies, from the smallest to the most massive ones, in all expected cosmological environments. We use gravity + magnetohydrodynamics simulations of large cosmological volumes. See more at the IllustrisTNG webpage
Cluster galaxies and evolution of galaxies in different environments
We use simulations to quantify the effects of environment into the evolution of galaxies, their star formation activity, morphologies, and stellar and gaseous content. For example, satellite galaxies orbiting within the potential well of massive galaxy clusters undergo stripping of their materials, including the gas which sometimes produce extended wakes.
Galaxy assembly, accreted stars and stellar haloes
Simulations have shown that galaxies assemble their stars by both making them (star formation) and by accreting and merging with other galaxies (accretion). Many of these accreted or ex-situ stars can be found at large distances around galaxies, forming the so called stellar haloes. We use simulations to quantify the assembly of galaxies and their stellar haloes across these different assembly channels, make predictions for future surveys and do comparisons to observations.
Assembly and properties of Milky Way like galaxies
One of the most intriguing challenges of our field is to understand our Galaxy, the Milky Way, and model all aspects of it. We use simulations (IllustrisTNG, Illustris and Eris) to understand how special our Galaxy is, how it formed and to interpret observational data from current Milky Way surveys.
Effects of baryons on (cold) dark matter
Simulations including only the effects of gravity (and hence only dark matter) have provided an exquisitely precise picture of the properties and distribution of dark matter, in haloes and across the large scale structure. However, recently, simulations including star formation, gas physics and feedback seem to suggest that such picture is more complex than anticipated…
Cosmology with eROSITA and the physics of galaxy clusters
eROSITA will be launched in the second half of 2018 and over the course of four years will return an unprecedented all-sky map of the X-ray universe, including about hundred of thousands galaxy clusters. These can be used to place constraints on our cosmological models, including the level and evolution of Dark Energy. In parallel, we can use simulations to quantify and predict the properties of the intra-cluster plasma, including its observational signatures as well as the effects of magnetic fields, shocks and feedback from the central super massive black holes.