Sloshing of the Magnetized Cool Gas in the Cores of Galaxy Clusters

Set Characteristics

  • Code: FLASH
  • Simulation type: AMR
  • Box size: L = 2 Mpc
  • Finest cell size: \(\Delta{x}_{\rm min}\) = 0.977 kpc
  • Primary cluster mass: \(M_{200} = 10^{15}~M_{\odot}\)


  • There is no metallicity field in these simulations; hence for computing X-ray emissivities a constant metallicity of \(Z = 0.3~Z_\odot\) is assumed.
  • The data presented here are not from the original simulations presented in the relevant paper but are improved versions with higher spatial resolution and improved treatment of gravity. For details on the latter see Roediger & ZuHone 2012.
  • For each simulation, the main cluster is fixed at r = [0, 0, 0] kpc. A tab-separated ASCII table containing the subcluster position, velocity, and acceleration as a function of time may be found here.



For non-cosmological simulations such as this one, a cosmology and redshift are assumed for the purposes of calculating distance and redshift-dependent quantities.

  • \(\Lambda{\rm CDM}\) cosmology
  • \(H_0 = 71~{\rm km~s^{-1}~Mpc^{-1}}\)
  • \(\Omega_m = 0.27\)
  • \(\Omega_\Lambda = 0.73\)
  • \(z = 0.05\) for all epochs


For the following simulations, \(\beta = p_{\rm th}/p_B\).


This set of simulations was performed using the Pleiades supercomputer at NASA’s Ames Research Center.