Abell 1142 galaksi kümesinin XMM-newton gözlemleri ve kimyasal analizi

A galaxy cluster is the physical assembly of multiple galaxies that are bound together by gravity. They may hold dozens to hundreds of galaxies with varying masses. However, these galaxies roughly represent only 20\% of the total baryonic mass within the cluster. The remaining 80\% is in the form of a superheated plasma that is ever-present throughout the cluster. This plasma is commonly called the ``Intracluster Medium" (ICM). The immense gravitational potential of the galaxy cluster heats the ICM to temperatures of a hundred million ($10^8$) kelvins, making the ICM a strong source of X-ray emissions. By looking at the X-ray spectra of the ICM, we can learn about its chemical composition and the processes that may have contributed to its chemical enrichment. Abell 1142 is a nearby ($z=0.035$), poor galaxy cluster that possesses two ``Brightest Cluster Galaxies" (BCG) with slightly varying velocities and an X-ray emission peak, which is located away from both BCGs and is also cooler than its surrounding ICM. While the former is typical for merging non-cool core clusters, the latter scenario is usually seen in relaxed, cool core clusters. This makes Abell 1142 (A1142) an interesting target for study. We aim to analyze the ICM around this X-ray peak, look at its temperature and chemical abundance profiles and discuss how the ICM of a cool core cluster might behave in the absence of an Active Galactic Nucleus (AGN) feedback.