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We characterize the non-sphericity of galaxy clusters by the projected axisratio of spatial distribution of star, dark matter, and X-ray surfacebrightness (XSB). We select 40 simulated groups and clusters of galaxies withmass larger than 5E13 Msun from the Horizon simulation that fully incorporatesthe relevant baryon physics, in particular, the AGN feedback. We find that thebaryonic physics around the central region of galaxy clusters significantlyaffects the non-sphericity of dark matter distribution even beyond the centralregion, approximately up to the half of the virial radius. Therefore it is verydifficult to predict the the probability density function (PDF) of theprojected axis ratio of XSB from dark-matter only N-body simulations asattempted in previous studies. Indeed we find that the PDF derived from oursimulated clusters exhibits much better agreement with that from the observedX-ray clusters. This indicates that our present methodology to estimate thenon-sphericity directly from the Horizon simulation is useful and promising.Further improvements in both numerical modeling and observational data willestablish the non-sphericity of clusters as a cosmological test complementaryto more conventional statistics based on spherically averaged quantities.

Projected Axis Ratios of Galaxy Clusters in the Horizon-AGN Simulation: Impact of Baryon Physics and Comparison with Observations