Halo Formation in Warm Dark Matter Models

Details Halo Formation in Warm Dark Matter Models Halo Formation in Warm Dark Matter Models

2000-10-19

arxiv.org/abs/astro-ph/0010389v3

Astrophys.J. 556 (2001) 93-107

Astronomy and Astrophysics

Astrophysics

37 pages, 13 postscript files. Higher resolution and color figures available at http://astro.princeton.edu/~bode/WDM/ . Accept

Scientific paper

10.1086/321541

Discrepancies have emerged between the predictions of standard cold dark matter (CDM) theory and observations of clustering on sub-galactic scales. Warm dark matter (WDM) is a simple modification of CDM in which the dark matter particles have initial velocities due either to their having decoupled as thermal relics, or having been formed via non-equilibrium decay. We investigate the nonlinear gravitational clustering of WDM with a high resolution N-body code, and identify a number of distinctive observational signatures. Relative to CDM, halo concentrations and core densities are lowered, core radii are increased, and large halos emerge with far fewer low mass satellites. The number of small halos is suppressed, and those present are formed by `top down' fragmentation of caustics, as part of a `cosmic web' connecting massive halos. Few small halos form outside this web. If we identify small halos with dwarf galaxies, their number, spatial distribution, and formation epoch appear in better agreement with the observations for WDM than they are for CDM.

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