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We use N-body simulations of dark matter haloes in cold dark matter (CDM) anda large set of different warm dark matter (WDM) cosmologies to demonstrate thatthe spherically averaged density profile of dark matter haloes has a shape thatdepends on the power spectrum of matter perturbations. Density profiles aresteeper in WDM but become shallower at scales less than one percent of thevirial radius. Virialization isotropizes the velocity dispersion in the innerregions of the halo but does not erase the memory of the initial conditions inphase space. The location of the observed deviations from CDM in the densityprofile and in phase space can be directly related to the ratio between thehalo mass and the filtering mass and are most evident in small mass haloes,even for a 34 keV thermal relic WDM. The rearrangement of mass within thehaloes supports analytic models of halo structure that include angularmomentum. We also find evidence of a dependence of the slope of the innerdensity profile in CDM cosmologies on the halo mass with more massive haloesexhibiting steeper profiles, in agreement with the model predictions and withprevious simulation results. Our work complements recent studies of microhaloesnear the filtering scale in CDM and strongly argue against a universal shapefor the density profile.

Fingerprints of the initial conditions on the density profiles of cold and warm dark matter haloes