Entropy plateaus can emerge from gas replacement at a characteristic halo mass in simulated groups and clusters of galaxies (2505.05675v1)

Abstract: The thermodynamic evolution of the intergalactic medium (IGM) is driven by a complex interplay between gravitational collapse, radiative cooling, and baryonic feedback associated with galaxy formation. Using cosmological hydrodynamic zoom-in simulations of a group of mass $8.83 \times 10^{12}$ M$\odot$ and a cluster of mass $2.92 \times 10^{14}$ M$\odot$ at $z=0$, we investigate the emergence of entropy plateaus at characteristic halo masses and their connection to feedback mechanisms. We use the SWIFT-EAGLE model with three resolution levels, down to an initial particle gas mass of $2.29 \times 10^5$ M$\odot$ and dark matter particle mass of $1.23 \times 10^6$ M$\odot$. Our analysis reveals that when halos reach $\sim 10^{12}$ M${\odot}$, their entropy profiles flatten at the virial radius, marking a transition where AGN feedback begins to dominate over supernova-driven regulation. By tracking the Lagrangian history of gas particles, we demonstrate that this entropy buildup is driven primarily by AGN feedback, which efficiently removes low-entropy gas from progenitors of groups and clusters, redistributing it throughout the IGM before the gas can fall into the core region. Recent XMM-Newton observations of X-GAP local groups reveal large entropy excesses and flat cores, in line with our predicted plateaus and in contrast to the steeper, power-law-like profiles of previous observations. While these predicted plateaus may be observationally confirmed in unbiased samples, reproducing the full diversity of entropy profiles, from flat cores to cool-core power laws, remains an outstanding challenge for next-generation feedback models. We suggest that current AGN feedback models may be overly efficient in expelling low-entropy gas from the potential cool-core $10^{12}$ M${\odot}$ progenitors, disrupting the balance between heating and cooling required to sustain long-lived cool cores.