Dynamical analysis of clusters of galaxies from cosmological simulations
  Studies of cluster mass and velocity anisotropy profiles are useful tests of
dark matter models, and of the assembly history of clusters of galaxies. These
studies might be affected by unknown systematics caused by projection effects.
We aim at testing observational methods for the determination of mass and
velocity anisotropy profiles of clusters of galaxies. Particularly, we focus on
the MAMPOSSt technique (Mamon et al. 2013).
  We use results from two semi-analytic models of galaxy formation coupled with
high-resolution N-body cosmological simulations, the catalog of De Lucia &
Blaizot (2007) and the FIRE catalog based on the new GAlaxy Evolution and
Assembly model.
  We test the reliability of the Jeans equation in recovering the true mass
profile when full projected phase-space information is available. We examine
the reliability of the MAMPOSSt method in estimating the true mass and velocity
anisotropy profiles of the simulated halos when only projected phase-space
information is available, as in observations.
  The spherical Jeans equation provides a reliable tool for the determination
of cluster mass profiles, also for subsamples of tracers separated by galaxy
color. Results are equally good for prolate and oblate clusters. Using only
projected phase-space information, MAMPOSSt provides estimates of the mass
profile with a standard deviation of 35-69 %, and a negative bias of 7-17 %,
nearly independent of radius, and that we attribute to the presence of
interlopers in the projected samples. The bias changes sign, that is, the mass
is over-estimated, for prolate clusters with their major axis aligned along the
line-of-sight. MAMPOSSt measures the velocity anisotropy profiles accurately in
the inner cluster regions, with a slight overestimate in the outer regions,
both for the whole sample of observationally-identified cluster members and
separately for red and blue galaxies.
