Speaker
Guilherme Pimentel
(Scuola Normale Superiore)
Description
I will describe a geometric picture for cosmological perturbation theory. Through this geometry, we can determine differential equations satisfied by these correlators, as functions of their momenta. In this ``holographic” picture, cosmological time evolution is encoded in a sort of Hamiltonian (a flat connection) in kinematic space. I will also show how to move away from the highly symmetric de Sitter arena, adding a twist which describes cosmological correlation functions for power-law FLRW cosmologies.
Author
Guilherme Pimentel
(Scuola Normale Superiore)
