The Effective Field Theory of Cosmological Large Scale Structures
  Large scale structure surveys will likely become the next leading
cosmological probe. In our universe, matter perturbations are large on short
distances and small at long scales, i.e. strongly coupled in the UV and weakly
coupled in the IR. To make precise analytical predictions on large scales, we
develop an effective field theory formulated in terms of an IR effective fluid
characterized by several parameters, such as speed of sound and viscosity.
These parameters, determined by the UV physics described by the Boltzmann
equation, are measured from N-body simulations. We find that the speed of sound
of the effective fluid is c_s^2 10^(-6) and that the viscosity contributions
are of the same order. The fluid describes all the relevant physics at long
scales k and permits a manifestly convergent perturbative expansion in the size
of the matter perturbations \delta(k) for all the observables. As an example,
we calculate the correction to the power spectrum at order \delta(k)^4. The
predictions of the effective field theory are found to be in much better
agreement with observation than standard cosmological perturbation theory,
already reaching percent precision at this order up to a relatively short scale
k \sim 0.24 h/Mpc.
