DE3 - Large Scale Structure and Statistics |
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Speaker |
Bruni, Marco |
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Coauthors |
Daniele Bertacca, Andrea Maselli, Irene Milillo, Daniel B. Thomas, David Wands |
| Talk Title |
Accounting for GR effects in large scale structure formation: a nonlinear post-Friedmann framework |
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Abstract |
Nonlinear structure formation at scales much smaller than the Hubble horizon is traditionally studied with Newtonian methods, for instance N-body simulations, while early Universe and horizon scales perturbations are investigated with relativistic perturbation theory. In view of new large scale galaxy surveys that will provide data with an unprecedented accuracy, it is timely to bridge the gap between these different approaches, going beyond the Newtonian approximation and unifying the study of the very large scales and the nonlinear scales in a single theoretical framework. In this talk I will briefly summarise recent work in perturbation theory on GR effects, then focusing on a novel approximation scheme in LCDM, the post-Friedmann framework. This is a sort of post-Minkowskian (weak field) approach to cosmology, fully nonlinear in the density field, such that at leading order in a 1/c expansion Newtonian cosmology is recovered as a consistent approximate solution of Einstein equations, on top of a Friedmannian background. In this post-Friedmann framework, linear and non-linear relativistic contributions appear at next order. Resumming variables and linearising the equations one recovers first-order relativistic perturbation theory, thus the framework is valid on horizon scales and beyond. I will illustrate the first practical application, i.e. the extraction of the frame-dragging gravitomagnetic potential from N-body simulations, and its power spectrum. Similarly, the difference between the two scalar potential, known as “slip” in cosmology, can also in principle be computed, sourced at leading order by purely Newtonian nonlinear terms. I will conclude with an outlook on further extensions and applications of this new formalism. |
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Talk view |
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