Kavli Affiliate: Debora Sijacki
| First 5 Authors: Jake S. Bennett, Debora Sijacki, , ,
| Summary:
The use of galaxy clusters as cosmological probes often relies on
understanding the properties and evolution of the intracluster medium (ICM).
However, the ICM is a complex plasma, regularly stirred by mergers and
feedback, with non-negligible bulk and turbulent motions and a non-thermal
pressure component, making it difficult to construct a coherent and
comprehensive picture. To this end, we use the FABLE simulations to investigate
how the hydrostatic mass bias is affected by mergers, turbulence, and feedback.
Following in detail a single, massive cluster we find the bias varies
significantly over cosmic time, rarely staying at the average value found at a
particular epoch. Variations of the bias at a given radius are contemporaneous
with periods where outflows dominate the mass flux, either due to mergers or
interestingly, at high redshift, AGN feedback. The $z=0$ ensemble median mass
bias in FABLE is $sim!13$ per cent at $R_mathrm{500}$ and $sim!15$ per
cent at $R_mathrm{200}$, but with a large scatter in individual values. In
halo central regions, we see an increase in temperature and a decrease in
non-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, to
estimate the bias, we find there can be significant differences, particularly
at larger radii and higher redshift. We therefore caution over the use of such
fits in future work when comparing with the next generation of X-ray and SZ
observations.
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