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The use of galaxy clusters as cosmological probes hinges on our ability tomeasure their masses accurately and with high precision. Hydrostatic mass isone of the most common methods for estimating the masses of individual galaxyclusters, which suffer from biases due to departures from hydrostaticequilibrium. Using a large, mass-limited sample of massive galaxy clusters froma high-resolution hydrodynamical cosmological simulation, in this work we showthat in addition to turbulent and bulk gas velocities, acceleration of gasintroduces biases in the hydrostatic mass estimate of galaxy clusters. Inunrelaxed clusters, the acceleration bias is comparable to the bias due tonon-thermal pressure associated with merger-induced turbulent and bulk gasmotions. In relaxed clusters, the mean mass bias due to acceleration is small(<3%), but the scatter in the mass bias can be reduced by accounting for gasacceleration. Additionally, this acceleration bias is greater in the outskirtsof higher redshift clusters where mergers are more frequent and clusters areaccreting more rapidly. Since gas acceleration cannot be observed directly, itintroduces an irreducible bias for hydrostatic mass estimates. Thisacceleration bias places limits on how well we can recover cluster masses fromfuture X-ray and microwave observations. We discuss implications for clustermass estimates based on X-ray, Sunyaev-Zeldovich effect, and gravitationallensing observations and their impact on cluster cosmology.

Weighing Galaxy Clusters with Gas. II. On the Origin of Hydrostatic Mass Bias in LambdaCDM Galaxy Clusters