  In this paper we examine how well galaxies and intra-cluster gas trace the
gravitational potential of clusters. Utilizing mass profiles derived from
gravitational lensing and X-ray observations, coupled with measured galaxy
velocities, we solve for the velocity anisotropy parameter using the
anisotropic Jeans equation. This is done for five clusters, three at low
redshift: A2199, A496 and A576 and two at high redshifts: A2390 and MS1358.
With X-ray temperature profiles obtained from Chandra and ASCA/ROSAT data, we
estimate the ratio of energy in the galaxies compared to the X-ray gas. We find
that none of these clusters is strictly in hydro-static equilibrium. We compare
the properties of our sample with clusters that form in high-resolution
cosmological N-body simulations that include baryonic physics. Simulations and
data show considerable scatter both these profiles. We demonstrate the future
feasibility and potential for directly comparing the orbital structure of
clusters inferred from multi-wavelength observations with high resolution
simulated clusters.
