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The use of galaxy clusters as cosmological probes often relies onunderstanding the properties and evolution of the intracluster medium (ICM).However, the ICM is a complex plasma, regularly stirred by mergers andfeedback, with non-negligible bulk and turbulent motions and a non-thermalpressure component, making it difficult to construct a coherent andcomprehensive picture. To this end, we use the FABLE simulations to investigatehow the hydrostatic mass bias is affected by mergers, turbulence, and feedback.Following in detail a single, massive cluster we find the bias variessignificantly over cosmic time, rarely staying at the average value found at aparticular epoch. Variations of the bias at a given radius are contemporaneouswith periods where outflows dominate the mass flux, either due to mergers orinterestingly, at high redshift, AGN feedback. The $z=0$ ensemble median massbias in FABLE is $\sim\!13$ per cent at $R_\mathrm{500}$ and $\sim\!15$ percent at $R_\mathrm{200}$, but with a large scatter in individual values. Inhalo central regions, we see an increase in temperature and a decrease innon-thermal pressure support with cosmic time as turbulence thermalises,leading to a reduction in the mass bias within $\sim\!0.2 \, R_\mathrm{200}$.When using a fitted pressure profile, instead of the simulation data, toestimate the bias, we find there can be significant differences, particularlyat larger radii and higher redshift. We therefore caution over the use of suchfits in future work when comparing with the next generation of X-ray and SZobservations.

A disturbing FABLE of mergers, feedback, turbulence, and mass biases in simulated galaxy clusters