Sayers, JackJackSayersSereno, MauroMauroSerenoETTORI, STEFANOSTEFANOETTORIRASIA, ELENAELENARASIACui, WeiguangWeiguangCuiGolwala, SunilSunilGolwalaUmetsu, KeiichiKeiichiUmetsuYepes, GustavoGustavoYepes2022-06-012022-06-0120210035-8711http://hdl.handle.net/20.500.12386/32161We report the non-thermal pressure fraction (P<SUB>nt</SUB>/P<SUB>tot</SUB>) obtained from a three-dimensional triaxial analysis of 16 galaxy clusters in the CLASH sample using gravitational lensing (GL) data primarily from Subaru and HST, X-ray spectroscopic imaging from Chandra, and Sunyaev-Zel'dovich effect (SZE) data from Planck and Bolocam. Our results span the approximate radial range 0.015-0.4 R<SUB>200m</SUB> (~35-1000 kpc). At cluster-centric radii smaller than 0.1 R<SUB>200m</SUB> the ensemble average P<SUB>nt</SUB>/P<SUB>tot</SUB> is consistent with zero with an upper limit of 9 per cent, indicating that heating from active galactic nuclei and other relevant processes does not produce significant deviations from hydrostatic equilibrium (HSE). The ensemble average P<SUB>nt</SUB>/P<SUB>tot</SUB> increases outside of this radius to approximately 20 per cent at 0.4 R<SUB>200m</SUB>, as expected from simulations, due to newly accreted material thermalizing via a series of shocks. Also in agreement with simulations, we find significant cluster-to-cluster variation in P<SUB>nt</SUB>/P<SUB>tot</SUB> and little difference in the ensemble average P<SUB>nt</SUB>/P<SUB>tot</SUB> based on dynamical state. We conclude that on average, even for diverse samples, HSE-derived masses in the very central regions of galaxy clusters require only modest corrections due to non-thermal motions.STAMPAen10.1093/mnras/stab1542https://academic.oup.com/mnras/article/505/3/4338/6287586?login=false2021MNRAS.505.4338SFIS/05 - ASTRONOMIA E ASTROFISICAERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_9 Clusters of galaxies and large scale structures