Issue EAS Publications Series Volume 20, 2006 Mass Profiles and Shapes of Cosmological Structures Page(s) 65 - 68 DOI 10.1051/eas:2006049 Published online 19 May 2006

Mass Profiles and Shapes of Cosmological Structures
G.A. Mamon, F. Combes, C. Deffayet and B. Fort (eds)
EAS Publications Series, 20 (2006) 65-68
DOI: 10.1051/eas:2006049

The Effect of Baryons on Halo Shapes

S. Kazantzidis^{1, 2}, A.R. Zentner² and D. Nagai<sup>2

1</sup>  Institute for Theoretical Physics, University of Zürich, 8057 Zürich, Switzerland
²  Kavli Institute for Cosmological Physics and Department of Astronomy and Astrophysics, The University of Chicago, Chicago, IL 60637, USA

Abstract

Using hydrodynamical cosmological simulations we investigate the effect of baryonic dissipation on halo shapes. We show that dissipational simulations produce significantly rounder halos than those formed in equivalent dissipationless simulations. Gas cooling causes an average increase in halo principal axis ratios of ~0.2-0.4 in the inner regions and a systematic shift that persists out to the virial radius, alleviating any tension between theory and observations. Although the magnitude of the effect may be overestimated due to overcooling, cluster formation simulations designed to reproduce the observed fraction of cold baryons still produce substantially rounder halos. Subhalos also exhibit a trend of increased axis ratios in dissipational simulations. Moreover, we demonstrate that subhalos are generally rounder than corresponding field halos even in dissipationless simulations. All of these results highlight the vital role of baryonic processes in comparing theory with observations and warn against over-interpreting discrepancies with collisionless simulations on small scales.

© EAS, EDP Sciences 2006

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