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We investigate the nonlinear evolution of structure in variants of thestandard cosmological model which display damped density fluctuations relativeto cold dark matter (e.g. in which cold dark matter is replaced by warm orinteracting DM). Using N-body simulations, we address the question of how muchinformation is retained from different scales in the initial linear powerspectrum following the nonlinear growth of structure. We run a suite of N-bodysimulations with different initial linear matter power spectra to show that,once the system undergoes nonlinear evolution, the shape of the linear powerspectrum at high wavenumbers does not affect the non-linear power spectrum,while it still matters for the halo mass function. Indeed, we find that linearpower spectra which differ from one another only at wavenumbers larger thantheir half-mode wavenumber give rise to (almost) identical nonlinear powerspectra at late times, regardless of the fact that they originate fromdifferent models with damped fluctuations. On the other hand, the halo massfunction is more sensitive to the form of the linear power spectrum. Exploitingthis result, we propose a two parameter model of the transfer function ingeneric damped scenarios, and show that this parametrisation works as well asthe standard three parameter models for the scales on which the linear spectrumis relevant.

Nonlinear growth of structure in cosmologies with damped matter fluctuations