English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Using high-resolution hydrodynamical simulations of galaxy clusters, we studythe interaction between the brightest cluster galaxy, its supermassive blackhole (BH) and the intracluster medium (ICM). We create initial conditions forwhich the ICM is in hydrostatic equilibrium within the gravitational potentialfrom the galaxy and an NFW dark matter halo. Two free parameters associatedwith the thermodynamic profiles determine the cluster gas fraction and thecentral temperature, where the latter can be used to create cool-core ornon-cool-core systems. Our simulations include radiative cooling, starformation, BH accretion, and stellar and active galactic nucleus (AGN)feedback. Even though the energy of AGN feedback is injected thermally andisotropically, it leads to anisotropic outflows and buoyantly rising bubbles.We find that the BH accretion rate (BHAR) is highly variable and onlycorrelates strongly with the star formation rate (SFR) and the ICM when it isaveraged over more than $1~\rm Myr$. We generally find good agreement with thetheoretical precipitation framework. In $10^{13}~\rm M_\odot$ haloes, AGNfeedback quenches the central galaxy and converts cool-core systems intonon-cool-core systems. In contrast, higher-mass, cool-core clusters evolvecyclically. Episodes of high BHAR raise the entropy of the ICM out to theradius where the ratio of the cooling time and the local dynamical time $t_{\rmcool}/t_{\rm dyn} > 10$, thus suppressing condensation and, after a delay, theBHAR. The corresponding reduction in AGN feedback allows the ICM to cool andbecome unstable to precipitation, thus initiating a new episode of high SFR andBHAR.

The interplay between AGN feedback and precipitation of the intracluster medium in simulations of galaxy groups and clusters