Formation and Evolution of
Galaxy Clusters Across Cosmic Time

There exist a variety of hydrodynamical codes, using different approaches to discretise gas and solve the hydrodynamical equations. All have different (dis)advantages. Meshless Finite Mass (MFM) is a new approach, combining a moving-mesh with SPH. We implement MFM into OpenGadget3 as an alternative to SPH. We test it's capabilities on idealised test cases and aim to compare, how it affects the evolution of galaxies / galaxy clusters. In this poster, we exemplary discuss two test-problems in more detail. Fluid-mixing instabilities can be calculated easily with MFM, even with a low order kernel, while SPH needs a high order kernel and thus a larger neighbor number. Nevertheless, the choice of the gradient limiter can significantly impact the evolution, and the best choice in general is not trivial. Decaying turbulence is a problem very hard to capture with many hydro-schemes. We show that MFM seems to work best and can capture the power spectrum well even at smaller scales. We conclude that MFM has several advantages over SPH and looks promising for the upcoming galaxy cluster simulations.