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Mass Estimation of Merging Galaxy Clusters

We investigate the impact of mergers on the mass estimation of galaxy clusters using N -body + hydrodynamical simulation data. We estimate the virial mass from these data and compare it with the real mass. When a smaller subcluster’s mass is larger than a quarter of that of the larger one, the virial mass can be larger than twice the real mass. The results strongly depend on the observational directions, because of an anisotropic velocity distribution of the member galaxies. We have also made X-ray surface brightness and spectroscopic-like temperature maps from the simulation data. The mass profile is estimated from these data on the assumption of hydrostatic equilibrium. In general, a mass estimation with X-ray data gives us better results than a virial mass estimation. The dependence upon observational directions is weaker than in the case of a virial mass estimation. When the system is observed along the collision axis, the projected mass tends to be underestimated. This fact should be noted, especially when