Spectral analysis of the a2384 galaxy cluster and the bridge between galaxy clusters

Galaxy clusters are massive structures bound by gravitational attraction, consisting of hundreds or even thousands of individual galaxies. As one of the largest structures in the universe, galaxy clusters are extremely rich in both ordinary (baryonic) and dark matter. The member galaxies within a galaxy cluster, along with dark matter and the hot gas spread throughout the cluster, are bound together under a significant gravitational potential. The hot gas found within galaxy clusters is called the "Intracluster Medium" (ICM), which, due to events like SNcc and SNIa supernova explosions occurring within the cluster, becomes chemically enriched and can reach temperatures of millions of degrees. This high temperature within the cluster causes the gas to emit strong X-rays, allowing us to study the temperature, metallicity, entropy, and chemical composition of the ICM through X-ray observations. In this study, the post-merger galaxy cluster known as Abell 2384 ($z \approx 0.0943$) is examined. The XMM-Newton/EPIC and Chandra/ACIS-I observations of the A2384(S) and A2384(N) clusters, as well as the bridge between them, have been analyzed, and temperature and metallicity profiles are presented. The models indicate that the Bridge 1 and Bridge 2 regions are hotter, more active, and more metal-rich compared to the A2384(S) and A2384(N) regions. Furthermore, models based on data obtained from Chandra and XMM-Newton observations show that the metallicity increases as one approaches the A2384(S) region, but this increase starts to decrease as one moves further into the A2384(S) region. This suggests the need for a more detailed investigation of the radio source mentioned in previous studies.