Structural and dynamical modeling of WINGS clusters

Numerical simulations indicate that cosmological halos display power-law radial profiles of pseudo phase-space density (PPSD), Q=rho/sigma^3, where rho is mass and sigma velocity dispersion. We test these predictions using the parameters derived from Markov Chain Monte Carlo (MCMC) analysis performed with MAMPOSSt code on observed kinematics a dispersion based stack (sigmav) 54 nearby regular clusters galaxies WINGS dataset. In definition PPSD, either in total (Q_rho) or galaxy number nu (Q_nu) three morphological classes (ellipticals, lenticulars, spirals), while (obtained by inversion Jeans equation) (Q_rho Q_nu) its component (Q_r,rho Q_r,nu). find PPSD are relations for nearly all MCMC parameters. The logarithmic slopes our Q_rho(r) Q_r,rho(r) ellipticals spirals excellent agreement particles simulations, but slightly shallower S0s. For Q_nu(r) Q_r,nu(r), only have slope matching much shallower, similar to subhalos. But cluster stacks richness gas temperature, fraction PPSDs lower (esp. Q_rho except profiles, defined rather than nu, appear be fundamental property clusters. They would imprinted during an early phase violent relaxation dark matter ellipticals, later as they move towards dynamical equilibrium gravitational potential, S0s intermediate (richness temperature-based stacks) mixed class (sigmav stack).