Effects of Angular Momentum on Halo Profiles
  The near universality of DM halo density profiles provided by N-body
simulations has proven to be robust against changes in total mass density,
power spectrum, and some forms of initial velocity dispersion. In this letter
we study the effects of coherently spinning up an isolated DM-only progenitor
on halo structure. Halos with spins within several standard deviations of the
simulated mean ($\lambda \lesssim 0.20$) produce profiles with negligible
deviations from the universal form. Only when the spin becomes quite large
($\lambda \gtrsim 0.20$) do departures become evident. The angular momentum
distribution also exhibits a near universal form, which is also independent of
halo spin up to $\lambda \lesssim 0.20$. A correlation between these epidemic
profiles and the presence of a strong bar in the virialized halo is also
observed. These bar structures bear resemblance to the radial orbit instability
in the rotationless limit.
