Sommaire:

In this talk, I will discuss some aspects of non-linear structure formation.
Calculations of correlation functions usually involve linear (relativistic) physics on large scales and non-linear (but Newtonian) physics on small scales. For the standard case of the 2-point correlation function, the relativistic effects remain small. However, for non-Gaussian signals, one needs to consider, the 3-point correlation function (the bispectrum) which couples large scales with small scales in the so-called squeezed limit. I will present the calculation of the non-linear relativistic corrections to the dynamics of dark matter and galaxy perturbations. The relativistic corrections are of the same order of magnitude, in the squeezed limit, than a primordial local non-Gaussianity signal. Such signal is expected to be within the accuracy of the next generation of LSS surveys. I will finally complement my study with some preliminary results of N-body simulations.

Pour plus d'informations, merci de contacter Poulin V.