Galaxy clusters offer celestial laboratories to study the evolution of the universe. Specifically, the intracluster medium (ICM) within them hosts an array of heavier elements, or metallicities, such as iron and nickel, that can be analyzed through their x-ray emission spectra. The goal of this research is to identify a correlation between the abundances of iron and nickel within the ICM in relation to the substructure of the galaxy clusters. Based on previous studies on the evolution of galaxy clusters (Anderson et. al 2009), I believe that a correlation exists between the abundance of iron and nickel and the morphologies of galaxy clusters. I used X-ray absorption spectroscopy to analyze the abundances of iron and nickel in these galaxy clusters. On my Linux system, I obtained a sample of 32 galaxy clusters with a redshift range 0.02<z<0.3 from the Chandra X-ray Observatory telescope that have corresponding values for morphology parameters in Parekh et. al 2015. Through using the Chandra X-ray Observatory's Ciao Tools analysis software and SAOImage DS9, I created a thermal plasma emission model (APEC) with a Bremsstrahlung Continuum model (TBABS) to obtain the abundances of the elements of iron and nickel. Subtle inaccuracies in the point source extraction for the galaxy clusters required filtering the abundance data through correlating its temperature vs. abundance with Baumgartner et. al 2005. I then correlated the data with the updated morphology parameters in Parekh et. al 2015 using Microsoft Excel. These parameters include the Gini coefficient, a measure of distribution of flux density from 0 most disturbed to I most relaxed, Moment of Light, a measure of the spatial distribution of multiple bright cores from -2.5 most relaxed to 0.7 most disturbed, and Concentration, the ratio of the percentage of x-ray flux from two distinct radii. After segregating my data based on the defined dynamical state of the cluster, I found a correlation between each parameter and the abundance of Fe and Ni for the non-relaxed clusters concluding that as a galaxy cluster becomes more disturbed in substructure, the abundances of Fe and Ni increase. The results were expected based on the cluster cooling time simulations from Parekh et. al 2015. As the cooling times increase for these clusters, the abundances of iron and nickel increase, asserting that as galaxy clusters mature, processes, such as star formation and supernovae occur producing heavier elements such as iron and nickel. To further confirm these findings, data of abundances for iron and nickel coupled with the data for morphological parameters from a higher redshift range can be analyzed. In addition, recent studies on the unidentified emission line from Bulbul et. al 2015 and others conclude that it is a signature of a sterile neutrino, which is a dark matter particle. Through studying abundance of this dark matter particle through X-ray absorption spectroscopy in relation to substructure parameters of galaxy clusters, we can better understand the influence dark matter has on the structure of baryonic matter within galaxy clusters.