Ewald Puchwein

TL;DR: Cosmological simulations of galaxy formation have been instrumental in advancing our understanding of structure and galaxy formation in the Universe as discussed by the authors, and have also proven useful to study alternative cosmological models and their impact on the galaxy population.

TL;DR: In this article, the authors used high-resolution cosmological simulations of a large cluster and group sample to study how BHs affect their host systems, including the halo gas fraction and the X-ray luminosity-temperature scaling relation, which are notoriously difficult to reproduce in self-consistent hydrodynamical simulations.

TL;DR: In this article, an energy-driven outflow model was proposed for galaxy formation in representative regions of the universe. But it is not a good fit for the observed galaxy stellar mass function, since the high-mass end can be recovered simultaneously with feedback from active galactic nuclei and a correction for diffuse stellar light plausibly missed in observations.

TL;DR: In this paper, the authors used a set of high-resolution hydrodynamical simulations of clusters of galaxies to study the build-up of the intracluster light (ICL), an interesting and likely significant component of their total stellar mass.

Abstract: We present a new massively parallel code for N-body and cosmological hydrodynamical simulations of modified gravity models. The code employs a multigrid-accelerated Newton-Gauss-Seidel relaxation solver on an adaptive mesh to efficiently solve for perturbations in the scalar degree of freedom of the modified gravity model. As this new algorithm is implemented as a module for the P-Gadget3 code, it can at the same time follow the baryonic physics included in P-Gadget3, such as hydrodynamics, radiative cooling and star formation. We demonstrate that the code works reliably by applying it to simple test problems that can be solved analytically, as well as by comparing cosmological simulations to results from the literature. Using the new code, we perform the first non-radiative and radiative cosmological hydrodynamical simulations of an f(R)-gravity model. We also discuss the impact of AGN feedback on the matter power spectrum, as well as degeneracies between the influence of baryonic processes and modifications of gravity.