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We use a set of 45 simulated clusters with a wide mass range ($8\times10^{13} < M_{500}~[$M$_{\odot}]~< 2\times 10^{15}$) to investigate the effectof varying hydrodynamics flavours on cluster mass estimates. The cluster zoomswere simulated using the same cosmological models as the BAHAMAS and C-EAGLEprojects, leading to differences in both the hydrodynamic solvers and thesubgrid physics but still producing clusters which broadly match observations.At the same mass resolution as BAHAMAS, for the most massive clusters ($M_{500}> 10^{15}$ M$_{\odot}$), we find changes in the SPH method produce the greatestdifferences in the final halo, while the subgrid models dominate at lower mass.By calculating the mass of all of the clusters using different permutations ofthe pressure, temperature and density profiles, created with either the truesimulated data or mock spectroscopic data, we find that the spectroscopictemperature causes a bias in the hydrostatic mass estimates which increaseswith the mass of the cluster, regardless of the SPH flavour used. For the mostmassive clusters, the estimated mass of the cluster using spectroscopic densityand temperature profiles is found to be as low as 50 per cent of the true masscompared to $\sim$ 90 per cent for low mass clusters. When including acorrection for non-thermal pressure, the spectroscopic hydrostatic massestimates are less biased on average and the mass dependence of the bias isreduced, although the scatter in the measurements does increase.

Hydrostatic mass estimates of massive galaxy clusters: a study with varying hydrodynamics flavours and non-thermal pressure support