MG13 - Talk detail

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Abstract

The analytical derivation of the structure and kinematics of self-gravitating, collisionless systems formed in hierarchical cosmologies is an old unresolved problem. In this contribution I present recent progress in this line. Making use of the old Secondary Infall model and under the assumption of inside-out growth of accreting haloes, contrasted with simulations, we derive the main properties of dark matter haloes directly from the power spectrum of density perturbations. This includes their triaxial shape, the spherically averaged density, velocity dispersion and velocity anisotropy profiles as well as their substructure. The model also holds for haloes having undergone major mergers. Applied to CDM cosmologies, this analytical approach allows one to solve important issues such as the logarithmic slope of the density profile at arbitrarily small radii or the origin of the power-law pseudo phase-space density profile and of the universal anisotropy profile shown by simulated haloes in CDM cosmologies. The application of the model to WDM cosmologies is also addressed.

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