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Fig. 2


The figure shows two distinct simulations from (MacMillan 2006). The right hand panels display the result (with continuing infall) of an isolated halo simulation starting from a set of particles perturbed by a cosmological spectrum of density and velocity fluctuations. The panel on the left indicates the same stage as developed from a non-perturbed halo. The upper line on the upper panel in each case is for a similar halo, but allowing only purely radial collapse. The middle line is the radial velocity dispersion while the lower line is the tangential dispersion. The lower panels display the anisotropy parameter for non-radial collapse.

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