Top-Down Fragmentation of a Warm Dark Matter Filament

Details Top-Down Fragmentation of a Warm Dark Matter Filament Top-Down Fragmentation of a Warm Dark Matter Filament

2003-02-21

arxiv.org/abs/astro-ph/0302443v2

Mon.Not.Roy.Astron.Soc. 345 (2003) 1285

Astronomy and Astrophysics

Astrophysics

7 pages, 7 figures, replaced with MNRAS accepted version (minor revisions)

Scientific paper

10.1046/j.1365-2966.2003.07044.x

We present the first high-resolution n-body simulations of the fragmentation of dark matter filaments. Such fragmentation occurs in top-down scenarios of structure formation, when the dark matter is warm instead of cold. In a previous paper (Knebe et al. 2002, hereafter Paper I), we showed that WDM differs from the standard Cold Dark Matter (CDM) mainly in the formation history and large-scale distribution of low-mass haloes, which form later and tend to be more clustered in WDM than in CDM universes, tracing more closely the filamentary structures of the cosmic web. Therefore, we focus our computational effort in this paper on one particular filament extracted from a WDM cosmological simulation and compare in detail its evolution to that of the same CDM filament. We find that the mass distribution of the halos forming via fragmentation within the filament is broadly peaked around a Jeans mass of a few 10^9 Msun, corresponding to a gravitational instability of smooth regions with an overdensity contrast around 10 at these redshifts. Our results confirm that WDM filaments fragment and form gravitationally bound haloes in a top-down fashion, whereas CDM filaments are built bottom-up, thus demonstrating the impact of the nature of the dark matter on dwarf galaxy properties.

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