The XRISM Resolve X-ray spectrometer allows to gain detailed insight into gas motions of the
intra cluster medium (ICM) of galaxy clusters. Current simulation studies focus mainly on statistical
comparisons, making the comparison to the currently still small number of clusters difficult due to
unknown selection effects. This study aims to bridge this gap, using simulated counterparts of Coma,
Virgo, and Perseus from the SLOW constrained simulations. These clusters show excellent agreement in
their properties and dynamical state with observations, thus providing an ideal testbed to understand
the processes shaping the properties of the ICM. We find that the simulations match the order of
the amount of turbulence for the three considered clusters, Coma being the most active, followed by
Perseus, while Virgo is very relaxed. Typical turbulent velocities are a few ≈100 km s−1, very close to
observed values. The resulting turbulent pressure support is ≈1% for Virgo, ≈6% for Perseus, and
≈8% for Coma within the central 1−2% of R200. Compared to previous simulations and observations,
measured velocities and turbulent pressure support are on average lower, in line with XRISM findings,
thus indicating the importance of selection effects.
