The slippery slope toward the bottom of the CMD hierarchy: Large-scale power's influence on ultra-small scale structure

Details The slippery slope toward the bottom of the CMD hierarchy: Large-scale power's influence on ultra-small scale structure The slippery slope toward the bottom of the CMD hierarchy: Large-scale power's influence on ultra-small scale structure

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006phdt.........5e&link_type=abstract

PhD Thesis: Proquest Dissertations And Theses 2006. Section 0283, Part 0606 108 pages; [M.Sc. dissertation].Canada: Queen's Univ

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N-body simulations are a vital tool in the study of structure formation and it is important to understand their limitations. In this thesis, we examine the effect of a finite simulation volume on Cold Dark Matter (CDM) structures and substructures. Our simulations were all carried out using standard cosmological models with a scale-free power-law spectra of density perturbations. We investigate a variety of spectral indices, corresponding to various scales in the standard CDM density perturbation spectrum, which becomes increasingly difficult to simulate as one approaches the bottom of the CDM hierarchy. Our approach is to normalize the spectrum so that the evolutionary state at a chosen mass scale remains unchanged as the box size is increased. We find that for a spectral index corresponding to galaxy cluster scales in the CDM spectrum, there is no change in the halo and subhalo population as the box size is doubled. At spectral indices corresponding to the sub-galactic scales, the halo number density is reduced by a factor of ~1.3 and the subhalo population is reduced by a factor of ~2 for every doubling of the box size. Moreover, the ability of a subhalo to survive is drastically reduced at small scales, going from a 32% accretion survival probability at galaxy cluster scales to less than 1% at the bottom of the CDM hierarchy. This means that N-body simulations at the bottom of the CDM hierarchy overestimate the subhalo number density by a factor of ~10 5 .

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