Stable clustering, the halo model and non-linear cosmological power spectra

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ID: 291226
2003
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Abstract
We present the results of a large library of cosmological N-body simulations, using power-law initial spectra. The nonlinear evolution of the matter power spectra is compared with the predictions of existing analytic scaling formulae based on the work of Hamilton et al. The scaling approach has assumed that highly nonlinear structures obey `stable clustering' and are frozen in proper coordinates. Our results show that, when transformed under the self-similarity scaling, the scale-free spectra define a nonlinear locus that is clearly shallower than would be required under stable clustering. Furthermore, the small-scale nonlinear power increases as both the power-spectrum index n and the density parameter Omega decrease, and this evolution is not well accounted for by the previous scaling formulae. This breakdown of stable clustering can be understood as resulting from the modification of dark-matter haloes by continuing mergers. These effects are naturally included in the analytic `halo model' for nonlinear structure; using this approach we are able to fit both our scale-free results and also our previous CDM data. This approach is more accurate than the commonly-used Peacock--Dodds formula and should be applicable to more general power spectra. Code to evaluate nonlinear power spectra using this method is available from http://as1.chem.nottingham.ac.uk/~res/software.html Following publication, we will make the power-law simulation data available through the Virgo website http://www.mpa-garching.mpg.de/Virgo
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Authors R. C. Smith, J. A. Peacock, Adrian Jenkins, Simon D. M. White, Carlos S. Frenk, F. R. Pearce, P. Thomas, G. Efstathiou, H. M. P. Couchman
Journal monthly notices of the royal astronomical society
Year 2003
DOI
10.1046/j.1365-8711.2003.06503.x
URL
https://academic.oup.com/mnras/article-pdf/341/4/1311/3500043/341-4-1311.pdf
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