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N. Rahman (IPAC/Caltech, USA), J. Krywult (Pedagogical University, Poland), P. Motl (Lousiana State University,USA), P. Flin (Pedagogical University, Poland), S. Shandarin (University of Kansas, USA)
We have made a comparative study of morphological evolution in simulated DM halos and X-ray brightness distribution and in optical clusters. Samples of simulated clusters include star formation with supernovae feedback, radiative cooling, and simulation in the adiabatic limit at three different redshifts, z = 0.0, 0.10, and 0.25. The optical sample contains 208 ACO clusters within redshift, z \leq 0.25. Cluster morphology, within 0.5 and 1.0 h-1 Mpc from cluster center, is quantified by multiplicity and ellipticity. In terms of multiplicity, our results indicate relatively stronger evolution in observed clusters than in the structure of simulated one. In terms of ellipticity, our results indicate slower increase in simulated cluster shapes with redshift compared to those in the observed one. We find that in some cases evolution in simulated clusters is consistent or even stronger than observed clusters, contrary to several recent studies. We notice that the different samples of observed clusters differ in morphological evolution with redshift. We highlight a few possibilities responsible for the discrepancy in the shape evolution of simulated and observed clusters.
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.