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Distribution and Evolution of Metals in the Magneticum Simulations

Universitäts-Sternwarte München, Faculty of Physics, Ludwig-Maximilians-Universität, Scheinerstr. 1, D-81679 München, Germany
Max Planck Institut for Astrophysics, D-85748 Garching, Germany
Author to whom correspondence should be addressed.
Academic Editors: Duncan A. Forbes and Ericson D. Lopez
Galaxies 2017, 5(3), 35;
Received: 30 June 2017 / Revised: 28 July 2017 / Accepted: 31 July 2017 / Published: 4 August 2017
(This article belongs to the Special Issue On the Origin (and Evolution) of Baryonic Galaxy Halos)
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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. View Full-Text
Keywords: galaxy clusters; intracluster medium; galaxies; stellar population; numerical simulation galaxy clusters; intracluster medium; galaxies; stellar population; numerical simulation

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Dolag, K.; Mevius, E.; Remus, R.-S. Distribution and Evolution of Metals in the Magneticum Simulations. Galaxies 2017, 5, 35.

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