The Perseus cluster of galaxies in X-rays Zoom Image
The Perseus cluster of galaxies in X-rays

High Energy Astrophysics

Galaxy Clusters

The group uses observational data and simulations to further the understanding of plasma in galaxies and galaxy clusters. Our investigations focus on the physics underlying the thermal state of the plasma, such as heat transfer, turbulence and viscosity, as well as the interplay of the plasma with active galactic nuclei.

Eugene Churazov's research focuses on studying plasma physics and cosmology using clusters of galaxies. Many basic properties of cluster plasma --- such as conduction, viscosity or the characteristics of turbulent gas motions --- remain unknown, while the abundance of clusters is directly linked to the properties of dark energy and dark matter. This makes cluster physics an exciting area of studies for the next decade.

Massimo Gaspari is dedicated to understanding the evolution of galaxy clusters and groups, via 3D MHD simulations. In particular, he is interested in various aspects of the ICM physics: radiative cooling, heating, isotropic/anisotropic conduction, instabilities, and multiphase gas. He performs detailed consistency tests with the latest observations in several bands, with X-ray data playing a central role.

Sergey Komarov studies the physics of the intracluster medium with Eugene Churazov. He is currently working on thermal conduction in the turbulent, magnetized plasma of cluster cores.

Natalya Lyskova is interested in determining the of masses and gravitational potentials of elliptical galaxies and galaxy clusters using different methods. Reliable mass estimates of individual galaxies and galaxy clusters play an important role in observational cosmology and studies of galaxy formation and evolution.

Irina Zhuravleva studies various physical processes in clusters of galaxies. The primary goal of the research is to understand and constrain properties of the velocity field by using (i) the resonant scattering effect and polarization in bright X-ray lines, (ii) fluctuations of the X-ray surface brightness, (iii) future observables to constrain the power spectrum of turbulence in the ICM and (iv) combined X-ray and optical observations to constrain the mass bias in clusters and massive ellipticals.

 
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