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The effect of AGN feedback on the brightest cluster elliptical galaxies


Matrizzi, D; Teyssier, R; Moore, B (2011). The effect of AGN feedback on the brightest cluster elliptical galaxies. In: Advances in Computational Astrophysics: Methods, Tools, and Outcome, Cefalu, Sicily, Italy, 13 June 2011 - 17 June 2011, 365.

Abstract

We show the properties of the Bright Central Galaxy (BCG) formed in the center of a Virgo-like cluster simulated using the AMR code RAMSES. We compared 2 models, with and without AGN feedback, showing that only the former can reproduce global properties of BCGs. It is possible to reproduce the stellar mass, the effective radius and the velocity dispersion of early-type galaxies in the field or in groups without considering AGN feedback, but the same properties of early-type galaxies in cluster sized halos are impossible to reproduce without AGN feedback. The strongest constraint comes from abundance matching, for which the stellar-to-halo mass ratio in simulations without AGN feedback appears too large when compared to observations. The kinematical and structural properties of the BCG are different in the two models. Without AGN feedback, we obtain a quickly rotating BCG, with high Sérsic index, a clear mass excess in the center and a very large stellar mass fraction. With AGN feedback, we obtain a slowly rotating BCG, with a significantly cored surface density profile and low stellar mass fraction.

Abstract

We show the properties of the Bright Central Galaxy (BCG) formed in the center of a Virgo-like cluster simulated using the AMR code RAMSES. We compared 2 models, with and without AGN feedback, showing that only the former can reproduce global properties of BCGs. It is possible to reproduce the stellar mass, the effective radius and the velocity dispersion of early-type galaxies in the field or in groups without considering AGN feedback, but the same properties of early-type galaxies in cluster sized halos are impossible to reproduce without AGN feedback. The strongest constraint comes from abundance matching, for which the stellar-to-halo mass ratio in simulations without AGN feedback appears too large when compared to observations. The kinematical and structural properties of the BCG are different in the two models. Without AGN feedback, we obtain a quickly rotating BCG, with high Sérsic index, a clear mass excess in the center and a very large stellar mass fraction. With AGN feedback, we obtain a slowly rotating BCG, with a significantly cored surface density profile and low stellar mass fraction.

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Additional indexing

Item Type:Conference or Workshop Item (Paper), not refereed, original work
Communities & Collections:07 Faculty of Science > Institute for Computational Science
Dewey Decimal Classification:530 Physics
Language:English
Event End Date:17 June 2011
Deposited On:14 Mar 2013 07:24
Last Modified:07 Dec 2017 18:09
Publisher:Astronomical Society of the Pacific
Series Name:Advances in Computational Astrophysics: Methods, Tools, and Outcome
Number:453
ISBN:978-1-58381-788-9
Official URL:http://aspbooks.org/custom/publications/paper/453-0365.html

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