Dark matter clustering: a simple renormalization group approach

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dc.creatorMcDonald, Patrick
dc.date2006-06-01
dc.date2006-12-30
dc.date.accessioned2026-07-07T10:23:09Z
dc.date.available2026-07-07T10:23:09Z
dc.descriptionI compute a renormalization group (RG) improvement to the standard beyond-linear-order Eulerian perturbation theory (PT) calculation of the power spectrum of large-scale density fluctuations in the Universe. At z=0, for a power spectrum matching current observations, lowest order RGPT appears to be as accurate as one can test using existing numerical simulation-calibrated fitting formulas out to at least k~=0.3 h/Mpc; although inaccuracy is guaranteed at some level by approximations in the calculation (which can be improved in the future). In contrast, standard PT breaks down virtually as soon as beyond-linear corrections become non-negligible, on scales even larger than k=0.1 h/Mpc. This extension in range of validity could substantially enhance the usefulness of PT for interpreting baryonic acoustic oscillation surveys aimed at probing dark energy, for example. I show that the predicted power spectrum converges at high k to a power law with index given by the fixed-point solution of the RG equation. I discuss many possible future directions for this line of work. The basic calculation of this paper should be easily understandable without any prior knowledge of RG methods, while a rich background of mathematical physics literature exists for the interested reader.
dc.descriptionmuch expanded explanation of basic calculation
dc.identifierhttps://arxiv.org/abs/astro-ph/0606028
dc.identifierhttp://arxiv.org/abs/astro-ph/0606028
dc.identifierPhys.Rev.D75:043514,2007
dc.identifierdoi:10.1103/PhysRevD.75.043514
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/175728
dc.subjectAstrophysics
dc.titleDark matter clustering: a simple renormalization group approach
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