Abstract
Metals are ideal tracers of the baryonic cycle within halos. Their composition is a fossil record connecting the evolution of the various stellar components of galaxies to the interaction with the environment by in- and out-flows. The Magneticum simulations allow us to study halos across a large range of masses and environments, from massive galaxy clusters containing hundreds of galaxies, down to isolated field galaxies. They include a detailed treatment of the chemo-energetic feedback from the stellar component and its evolution, as well as feedback from the evolution of supermassive black holes. Following the detailed evolution of various metal species and their relative composition due to continuing enrichment of the IGM and ICM by SNIa, SNII and AGB winds of the evolving stellar population is revealed the complex interplay of local star-formation processes, mixing, global baryonic flows, secular galactic evolution and environmental processes. We present results from the Magneticum simulations on the chemical properties of simulated galaxies and galaxy clusters, carefully comparing them to observations. We show that the simulations already reach a very high level of realism within their complex descriptions of the chemo-energetic feedback, successfully reproducing a large number of observed properties and scaling relations. Our simulated galaxies clearly indicate that there are no strong secondary parameters (such as star-formation rates at a fixed redshift) driving the scatter in these scaling relations. The remaining differences clearly point to detailed physical processes, which have to be included in future simulations.
Highlights
In cosmological hydrodynamical simulations, star formation is typically treated as based on a sub-grid model
Each star particle emits a feedback that mimicks the winds that are launched by stars in reality by averaging over the whole stellar population included in each simulated stellar particle
Metals are measured in all phases of the baryonic universe, starting from the inter-cluster medium (ICM) in galaxy clusters down to gas and stars in individual galaxies
Summary
Star formation is typically treated as based on a sub-grid model. Stars with masses larger than 8 M are believed to end their lives through a “core collapse” (SNII), typically releasing an energy of 1051 erg per supernova together with their chemical imprint into the surrounding gas These supernovae usually occur shortly after the formation of the simulated star particle, as the most massive stars only live for a short time, and this part of the stellar population. To include the effects of these sources in the sub-grid models of simulated stellar particles raises the need to integrate a set of complicated equations describing the evolution of a simple stellar population Such a set of integral equations allows us to compute at each time the rate at which the current AGB stars pollute their environment by stellar winds and the rate at which the SNIa and SNII are exploding. We will summarize and discuss the results of this comparison in the light of model improvements needed for the future
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