Simulating Astro-E2 Observations of Galaxy Clusters: the Case of   Turbulent Cores Affected by Tsunamis
  This is the first attempt to construct detailed X-ray spectra of clusters of galaxies from the results of high-resolution hydrodynamic simulations and simulate X-ray observations in order to study velocity fields of the intracluster medium (ICM). The hydrodynamic simulations are based on the recently proposed tsunami model, in which cluster cores are affected by bulk motions of the ICM and turbulence is produced. We note that most other solutions of the cooling flow problem also involve the generation of turbulence in cluster cores. From the mock X-ray observations with Astro-E2 XRS, we find that turbulent motion of the ICM in cluster cores could be detected with the satellite. The Doppler shifts of the metal lines could be used to discriminate among turbulence models. The gas velocities measured through the mock observations are consistent with the line-emission weighted values inferred directly from hydrodynamic simulations. 
Yutaka Fujita (1), Tomoaki Matsumoto (2), Keiichi Wada (1), and Tae   Furusho (3) ((1) NAOJ, (2) Hosei U., (3) ISAS/JAXA)