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Galaxy cluster mass determinations achieved using X-ray andSunyaev-Zel'dovich data combined with the assumption of hydrostatic equilibriumare generally biased. The bias exists for two main reasons: non-thermalpressure forces are expected to contribute to the overall pressure balance anddeviations from spherical symmetry and hydrostatic equilibrium can be present.In this paper, we use a sample of zoom-in hydrodynamical simulations of galaxyclusters to measure the magnitude of hydrostatic bias and the non-thermalcontribution to the total pressure. We propose a new empirical model fornon-thermal pressure based on our simulations that can be applied toobservations. We show that our model can be successfully applied to remove mostof the bias related to neglection of non-thermal pressure, which is usually notincluded in hydrostatic cluster mass profile reconstructions. The use of thismodel may significantly improve the calibration of cluster scaling relationsthat are a key tool for cluster cosmology.

Mass modeling of galaxy clusters: quantifying hydrostatic bias and contribution from non-thermal pressure