The evolution substructure I: a new identification method

Details The evolution substructure I: a new identification method The evolution substructure I: a new identification method

2004-04-13

arxiv.org/abs/astro-ph/0404258v1

Mon.Not.Roy.Astron.Soc. 351 (2004) 399

Astronomy and Astrophysics

Astrophysics

12 pages, 10 figures, MNRAS in press, the halo finder MHF is available from http://astronomy.swin.edu.au/MLAPM

Scientific paper

10.1111/j.1365-2966.2004.07786.x

We describe our new "MLAPM-halo-finder" (MHF) which is based on the adaptive grid structure of the N-body code MLAPM. We then extend the MHF code in order to track the orbital evolution of gravitationally bound objects through any given cosmological N-body simulation - our so-called "MLAPM-halo-tracker" (MHT). The mode of operation of MHT is demonstrated using a series of eight high-resolution N-body simulations of galaxy clusters. Each of these halos hosts more than one million particles within their virial radii Rvir. We use MHT as well as MHF to follow the temporal evolution of hundreds of individual satellites, and show that the radial distribution of these substructure satellites follows a "universal" radial distribution irrespective of the host halo's environment and formation history. This in fact might pose another problem for simulations of CDM structure formation as there are recent findings by Taylor et al. (2003) that the Milky Way satellites are found preferentially closer to the galactic centre and simulations underestimate the amount of central substructure, respectively. Further, this universal substructure profile is anti-biased with respect to the underlying dark matter profile. Both the halo finder MHF and the halo tracker MHT will become part of the open source MLAPM distribution.

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