Abstract

Recent spectral and spatial X-ray observations of galaxy clusters suggest subclustering and merging are common phenomena. Galaxy clusters can therefore be grouped into two categories: relaxed and nonrelaxed. Investigating cluster dynamical states is vital because it is linked with the evolution of galaxy clusters on cosmic time scales. It affects cluster global properties such as the virial temperature, metal distribution, luminosity, and mass calculation. We have investigated the use of a number of morphological parameters (Gini, Asymmetry, M20, Concentration, Ellipticity, Smoothness and Gini 2^nd order) to differentiate between relaxed and non-relaxed scenarios. We initially simulated different relaxed and nonrelaxed morphologies with multiple beta profiles. Finally, we applied our method to a different redshift sample of clusters from the Chandra archive and studied correlations between parameters and X-ray gas properties. In this proceding, we will show the promising results from the quantitative study of morphology parameters and its possible application to study the morphology of radio halos and relics clusters.