ETTORI, STEFANOSTEFANOETTORIEckert, D.D.Eckert2025-01-202025-01-2020220004-6361http://hdl.handle.net/20.500.12386/35654We present a modelization of the non-thermal pressure, $P_{NT}$, and we apply it to the X-ray (and Sunayev-Zel'dovich) derived radial profiles of the X-COP galaxy clusters. We relate the amount of non-thermal pressure support to the hydrostatic bias, $b$, and speculate on how we can interpret this $P_{NT}$ in terms of the expected levels of turbulent velocity and magnetic fields. Current upper limits on the turbulent velocity in the intracluster plasma are used to build a distribution $\mathcal{N}(<b) - b$, from which we infer that 50 per cent of local galaxy clusters should have $b < 0.2$ ($b<0.33$ in 80 per cent of the population). The measured bias in the X-COP sample that includes relaxed massive nearby systems is 0.03 in 50% of the objects and 0.17 in 80% of them. All these values are below the amount of bias required to reconcile the observed cluster number count in the cosmological framework set from Planck.STAMPAenArticle10.1051/0004-6361/2021426382-s2.0-85122227933http://arxiv.org/abs/2112.07554v1https://www.aanda.org/articles/aa/full_html/2022/01/aa42638-21/aa42638-21.htmlFIS/05 - ASTRONOMIA E ASTROFISICA