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Proposing Institution

ITA Heidelberg
Project Manager

Dr. Luigi Iapichino
Albert-Ueberle-Str. 2
69120 Heidelberg
The hot gas in galaxy clusters reaches temperatures of order 10^7...10^9 K. While it has been studied in detail how the spatial temperature structure of the intracluster gas can be understood, it remains an open question how clusters individually and as a population heat up in the course of cosmic history. This question is interesting because some of the most important observational signatures of galaxy clusters, in particular their X-ray emission and the thermal Sunyaev-Zel'dovich effect through which they appear in the sub-mm regime, hinge on their thermal history. As the most massive gravitationally bound structures in the Universe, clusters can be seen as index fossils of the cosmic evolution. Their evolution in the distant Universe can be expected to provide most valuable information on cosmic structure formation, and thus on dark matter and dark energy alike. We are proposing to study with numerical simulations how different heating mechanisms proposed in the literature can act, what quantitative role they play individually and jointly and whether they allow a complete understanding of cluster heating. In particular, we intend to study spherical and aspherical smooth accretion, infall of sublumps of different masses and the inflow of cold gas along filaments, both with idealized setups and full cosmological simulations.

Impressum, Conny Wendler