Non-linear evolution of suppressed dark matter primordial power spectra

Details Non-linear evolution of suppressed dark matter primordial power spectra Non-linear evolution of suppressed dark matter primordial power spectra

Jun 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005mnras.360..282b&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 360, Issue 1, pp. 282-287.

Astronomy and Astrophysics

Astronomy

5

Methods: N-Body Simulations, Cosmology: Theory, Dark Matter, Large-Scale Structure Of Universe

Scientific paper

We address the degree and rapidity of generation of small-scale power over the course of structure formation in cosmologies where the primordial power spectrum is strongly suppressed beyond a given wavenumber. We first summarize the situations where one expects such suppressed power spectra and point out their diversity. We then employ an exponential cut-off, which characterizes warm dark matter (WDM) models, as a template for the shape of the cut-off and focus on damping scales ranging from 106 to 109h-1Msolar. Using high-resolution simulations, we show that the suppressed part of the power spectrum is quickly (re)generated and catches up with both the linear and the non-linear evolution of the unsuppressed power spectrum. From z= 2 onwards, a power spectrum with a primordial cut-off at 109h-1Msolar becomes virtually indistinguishable from an evolved cold dark matter (CDM) power spectrum. An attractor such as that described in Zaldarriaga, Scoccimarro & Hui for power spectra with different spectral indices also emerges in the case of truncated power spectra. Measurements of z~ 0 non-linear power spectra at ~100h-1kpc cannot rule out the possibility of linear power spectra damped below ~109h-1Msolar. Therefore, WDM or scenarios with similar features should be difficult to exclude in this way.

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