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Fig. 6.

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Dependence of the X-ray-inferred velocity dispersion of the ICM on cluster mass (M200c) and central SMBH properties according to TNG-Cluster. For the latter, we show SMBH mass (MBH, the single largest in each halo), instantaneous accretion rate (BH), and accumulated kinetic feedback energy (Ekin). The solid (dashed) line represents the best-fit linear relation between the spectral-fitting (mass-weighted) velocity dispersion and cluster mass or SMBH properties. Cool-core clusters in the Perseus mass range exhibit larger levels of turbulence if they host a more massive SMBH, a SMBH that is accreting at higher rates, or a SMBH that has released more kinetic feedback on its surroundings throughout its life time.

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