Hostname: page-component-cd9895bd7-jn8rn Total loading time: 0 Render date: 2024-12-25T16:11:08.586Z Has data issue: false hasContentIssue false
  • English
  • Français

The role of Active Galactic Nuclei feedback in the formation of the brightest cluster galaxies

Published online by Cambridge University Press:  17 July 2013

Davide Martizzi ,
Romain Teyssier  and
Ben Moore
Davide Martizzi
Affiliation:
Institute for Theoretical Physics, University of Zurich, CH-8057 Zürich, Switzerland email: [email protected], [email protected], [email protected]
Romain Teyssier
Affiliation:
Institute for Theoretical Physics, University of Zurich, CH-8057 Zürich, Switzerland email: [email protected], [email protected], [email protected] CEA Saclay, DSM/IRFU/SAP, Bâtiment 709, F-91191 Gif-sur-Yvette, Cedex, France
Ben Moore
Affiliation:
Institute for Theoretical Physics, University of Zurich, CH-8057 Zürich, Switzerland email: [email protected], [email protected], [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The formation of the brightest cluster galaxies (BCG) is a challenge for galaxy formation theory. We performed high resolution cosmological hydrodynamical simulations with the AMR code RAMSES to study the properties of the BCG which forms at the center of a Virgo–like cluster. We compare the results of 2 galaxy formation scenarios, one in which only supernovae feedback is included, and one in which also AGN feedback is considered. Properties of the simulated BCG which are comparable with those of observed massive elliptical galaxies and BCGs cannot be obtained if AGN feedback is not considered. The stellar-to-halo mass ratio in simulations without AGN feedback appears too large when compared to observations, while it is compatible the observationally determined values when AGN feedback is included. The kinematical and structural properties of the BCG are extremely different in the two models. When we do not include AGN feedback, the BCG is quickly rotating, with high Sérsic index, a clear mass excess in the center and a very large stellar mass fraction. When AGN feedback is considered, the BCG is slowly rotating, with a significantly cored surface density profile and low stellar mass fraction.

Keywords

Galaxy Formation – TheoryGalaxy ClustersBlack HolesCosmologyNumerical Methods
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S295: The intriguing life of massive galaxies , August 2012 , pp. 362 - 365
Copyright
Copyright © International Astronomical Union 2013 

References

Teyssier, R. 2002, A&A, 385, 337Google Scholar
Booth, C. M. & Schaye, J. 2009, MNRAS, 398, 53Google Scholar
Naab, T., Johansson, P. H., & Ostriker, J. P. 2009, ApJ, 699, L178Google Scholar
Feldmann, R., Carollo, C. M., Mayer, L., et al. 2010, ApJ, 709, 218Google Scholar
Martizzi, D., Teyssier, R., & Moore, B. 2012, MNRAS, 420, 2859CrossRefGoogle Scholar
Moster, B. P., Somerville, R. S., Maulbetsch, C., et al. 2010, ApJ, 710, 903Google Scholar
Brough, S., Tran, K.-V., Sharp, R. G., von der Linden, A., & Couch, W. J. 2011, MNRAS, 414, L80Google Scholar
van der Wel, A., Holden, B. P., Zirm, A. W., et al. 2008, ApJ, 688, 48Google Scholar
Martizzi, D., Teyssier, R., Moore, B., & Wentz, T. 2012, MNRAS, 422, 3081Google Scholar