Description
Galaxy clusters are the largest gravitationally bound systems in the universe and serve as powerful laboratories for studying cosmology and astrophysical processes. Hydrodynamical simulations provide crucial insights into their formation, evolution, and the complex interplay between dark matter, gas dynamics, and feedback mechanisms. Galaxy clusters are often modeled as spherically symmetric systems, yet their true shapes are frequently ellipsoidal, especially in the case of dynamically unrelaxed clusters undergoing mergers. This assumption can lead to biases in key derived properties, such as pressure profiles, particularly when using standard spherical fitting techniques for clusters going through mergers. In this study, high-mass clusters from the MACSIS hydrodynamical simulation catalogue are analysed to investigate whether adopting an ellipsoidal modeling approach leads to a better characterization of the generalized Navarro-Frenk-White (gNFW) pressure profile. Given that major mergers and presence of substructure introduce asymmetries in the intracluster medium (ICM), we expect that ellipsoidal models will better capture the cluster morphology and reduce fitting residuals. The resulting parameters obtained by fitting pressure profiles for the spherical and ellipsoidal models are compared to assess the goodness-of-fit in both the cases.
