The matter power spectrum in redshift space using effective field theory
  The use of Eulerian 'standard perturbation theory' to describe mass assembly
in the early universe has traditionally been limited to modes with k $\lesssim$
0.1 h/Mpc at z = 0. At larger k the SPT power spectrum deviates from
measurements made using N-body simulations. Recently, there has been progress
in extending the reach of perturbation theory to larger k using ideas borrowed
from effective field theory. We revisit the computation of the redshift-space
matter power spectrum within this framework, including for the first time the
full one-loop time dependence. We use a resummation scheme proposed by Vlah et
al. to account for damping of baryonic acoustic oscillations due to large-scale
random motions and show that this has a significant effect on the multipole
power spectra. We renormalize by comparison to a suite of custom N-body
simulations matching the MultiDark MDR1 cosmology. At z = 0 and for scales k
$\lesssim$ 0.4 h/Mpc we find that the EFT furnishes a description of the
real-space power spectrum up to $\sim$2%, for the $\ell$ = 0 mode up to
$\sim$5%, and for the $\ell$ = 2, 4 modes up to $\sim$25%. We argue that, in
the MDR1 cosmology, positivity of the $\ell$ = 0 mode gives a firm upper limit
of k $\approx$ 0.75 h/Mpc for the validity of the one-loop EFT prediction in
redshift space using only the lowest-order counterterm. We show that replacing
the one-loop growth factors by their Einstein-de Sitter counterparts is a good
approximation for the $\ell$ = 0 mode, but can induce deviations as large as 2%
for the $\ell$ = 2, 4 modes. An accompanying software bundle, distributed under
open source licenses, includes Mathematica notebooks describing the
calculation, together with parallel pipelines capable of computing both the
necessary one-loop SPT integrals and the effective field theory counterterms.
