On the βSPEC Values of Galaxy Clusters During the Merger

Time-dependent, X-ray emission properties of merging subclusters of galaxies are studied by N-body + Hydrodynamic simulations. We consider rather idealized cases, in which two virialized subclusters with the same or different masses collide with each other, eventually merging into one bigger cluster. We find that the various observable quantities, such as the cluster temperature, T_g, the line-of-sight velocity dispersion of galaxies, σ₁, and the specific energy ratio, β_spec ≡ μ m_p σ /k_B T_g (where μ is the mean molecular weight in amu, m_p is the proton mass and k_B is the Boltzmann constant) are distinct in merging clusters from those in isolated clusters. When merging, especially, in addition to having large velocity dispersions, σ_l ≳ 2000 km s^-1, clusters will have large deviations of β_spec from unity; that is, β_spec ≳ 2.0 (or β_spec ≲ 0.5) when seen from the direction parallel (perpendicular) to the collision axis. Temperature profiles are the best indicator of merging process. The calculated temperature maps of merging clusters are compared with those of the observed clusters, such as the Coma cluster, A754, and A401/399 supercluster. These simulated features are in good agreement with what ASCA revealed. Further, we present rather unique features in the temperature profiles that can be caused by a merger (or an encounter) with a subgroup of galaxies. This revised version was published online in July 2006 with corrections to the Cover Date.