Merger Histories in Warm Dark Matter Structure Formation Scenario

Details Merger Histories in Warm Dark Matter Structure Formation Scenario Merger Histories in Warm Dark Matter Structure Formation Scenario

2001-05-17

arxiv.org/abs/astro-ph/0105316v2

Mon.Not.Roy.Astron.Soc. 329 (2002) 813

Astronomy and Astrophysics

Astrophysics

11 pages, 17 figures, MNRAS submitted, high-res figures can be found at http://www-thphys.physics.ox.ac.uk/users/AlexanderKneb

Scientific paper

10.1046/j.1365-8711.2002.05017.x

Observations on galactic scales seem to be in contradiction with recent high resolution N-body simulations. This so-called cold dark matter (CDM) crisis has been addressed in several ways, ranging from a change in fundamental physics by introducing self-interacting cold dark matter particles to a tuning of complex astrophysical processes such as global and/or local feedback. All these efforts attempt to soften density profiles and reduce the abundance of satellites in simulated galaxy halos. In this paper, we explore a somewhat different approach which consists of filtering the dark matter power spectrum on small scales, thereby altering the formation history of low mass objects. The physical motivation for damping these fluctuations lies in the possibility that the dark matter particles have a different nature i.e. are warm (WDM) rather than cold. We show that this leads to some interesting new results in terms of the merger history and large-scale distribution of low mass halos, as compared to the standard CDM scenario. However, WDM does not appear to be the ultimate solution, in the sense that it is not able to fully solve the CDM crisis, even though one of the main drawbacks, namely the abundance of satellites, can be remedied. Indeed, the cuspiness of the halo profiles still persists, at all redshifts, and for all halos and sub-halos that we investigated. Despite the persistence of the cuspiness problem of DM halos, WDM seems to be still worth taking seriously, as it alleviates the problems of overabundant sub-structures in galactic halos and possibly the lack of angular momentum of simulated disk galaxies. WDM also lessens the need to invoke strong feedback to solve these problems, and may provide a natural explanation of the clustering properties and ages of dwarfs.

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