A universal angular momentum profile for galactic halos

We study the angular momentum profiles of a statistical sample of halos dra wn from a high-resolution N-body simulation of the Lambda CDM cosmology. We find that the cumulative mass distribution of specific angular momentum j in a halo of mass M-v is well fitted by a universal function, M(<j) = M-v<m u>j/(j(0) + j). This profile is defined by one shape parameter (mu or j(0)) in addition to the global spin parameter lambda. It follows a power law M( <j) <proportional to> j over most of the mass and flattens at large j, with the flattening more pronounced for small values of mu (or large j(0) at a fixed lambda). Compared to a uniform sphere in solid-body rotation, most ha los have a higher fraction of their mass in the low- and high-j tails of th e distribution. High-lambda halos tend to have high mu values, correspondin g to a narrower, more uniform j distribution. The spatial distribution of a ngular momentum in halos tends to be cylindrical and is well-aligned within each halo for similar to 80% of the halos. The more misaligned halos tend to have low mu values. When averaged over spherical shells encompassing mas s M, the halo j profiles are fitted by j(M) proportional to M-s with s = 1. 3 +/- 0.3. We investigate two ideas for the origin of this profile. The fir st is based on a revised version of linear tidal-torque theory combined wit h extended Press-Schechter mass accretion, and the second focuses on j tran sport in minor mergers. Finally, we briefly explore implications of the M(< j) profile on the formation of galactic disks assuming that j is conserved during an adiabatic baryonic infall. The implied gas density profile deviat es from an exponential disk, with a higher density at small radii and a tai l extending to large radii. The steep central density profiles may imply di sk scale lengths that are smaller than observed. This is reminiscent of the "angular momentum problem" seen in hydrodynamic simulations, even though w e have assumed perfect j conservation. A possible solution is to associate the central excesses with bulge components and the outer regions with exten ded gaseous disks.