Kinetic structure of the intracluster medium across nearby clusters observed with XRISM

The X-Ray Imaging and Spectroscopy Mission (XRISM)/Resolve is building a sample of galaxy clusters with directly measured intracluster medium (ICM) gas motions, revealing diverse projected dynamical states. We compile 45 XRISM/Resolve measurements in 19 nearby galaxy clusters and place them on a common, emission-weighted effective line-of-sight scale, eff. We compare the line-of-sight velocity dispersion σ ᵥ, bulk velocity amplitude |vbulk|, their ratio Rᵥ ≡ |vbulk|/σ ᵥ, and nonthermal pressure proxies. Disturbed non-cool-core systems are not simply higher-dispersion counterparts of relaxed cool-core regions. Instead, differences among cool-core centers, cool-core outer regions, and non-cool-core systems are driven mainly by coherent line-of-sight motion relative to unresolved line broadening: Rᵥ tends to remain below unity in cool-core regions but often exceeds unity in non-cool-core systems, with the mean Rᵥ rising from 0.45 in cool-core centers to 1.6 in non-cool-core systems. These diagnostics help separate local central line broadening, likely associated with active galactic nuclei feedback in some cool cores, from larger-scale coherent motions associated with sloshing, mergers, and halo assembly. Comparison with forward-modeled TNG-Cluster predictions from the IllustrisTNG (TNG) simulation suite suggests that many cool-core measurements occupy the lower part of the predicted nonthermal pressure range, consistent with small hydrostatic-mass corrections in relaxed systems and larger corrections in disturbed ones. XRISM is thus beginning to resolve the projected kinetic structure of the ICM across cluster environments, rather than tracing a single sequence of increasing turbulence.