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The dynamical evolution of galaxy clusters taking into account the deceleration of disk galaxies by the gaseous component of the cluster

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Abstract

Numerical simulations of the dynamical evolution of a galaxy cluster in the framework of the N-body problem taking into account dark matter are presented. These simulations are aimed at studying the role of intergalactic gas in the cluster (the ICM) in the formation of a central, supermassive cD galaxy. The numerical models indicate that deceleration of the galaxies by intergalactic gas supports the observed high temperature of this gas, and accelerates the formation of a supermassive cD galaxy in the cluster core. The accretion of interstellar gas by the cluster core can support a high accretion rate by the central, supermassive black hole associated with the nucleus of the cD galaxy. As a result, this nucleus harbors a bright quasar. The mass of the black hole can grow with time to values 1010 M ⊙, as are observed for the brightest quasars.

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Authors and Affiliations

  1. Gorkii Ural State University, Yekaterinburg, Russia

    G. N. Dremova & V. V. Dremov

  2. Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia

    A. V. Tutukov

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  1. G. N. Dremova
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  2. A. V. Tutukov
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  3. V. V. Dremov
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Original Russian Text © G.N. Dremova, A.V. Tutukov, V.V. Dremov, 2010, published in Astronomicheskiĭ Zhurnal, 2010, Vol. 87, No. 8, pp. 768–783.

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Dremova, G.N., Tutukov, A.V. & Dremov, V.V. The dynamical evolution of galaxy clusters taking into account the deceleration of disk galaxies by the gaseous component of the cluster. Astron. Rep. 54, 704–718 (2010). https://doi.org/10.1134/S1063772910080032

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