Revising the Halofit Model for the Nonlinear Matter Power Spectrum
  Based on a suite of state-of-the-art high-resolution $N$-body simulations, we
revisit the so-called halofit model (Smith et al. 2003) as an accurate fitting
formula for the nonlinear matter power spectrum. While the halofit model has
been frequently used as a standard cosmological tool to predict the nonlinear
matter power spectrum in a universe dominated by cold dark matter, its
precision has been limited by the low-resolution of $N$-body simulations used
to determine the fitting parameters, suggesting the necessity of improved
fitting formula at small scales for future cosmological studies. We run
high-resolution $N$-body simulations for 16 cosmological models around the
Wilkinson Microwave Anisotropy Probe (WMAP) best-fit cosmological parameters
(1, 3, 5, and 7 year results), including dark energy models with a constant
equation of state. The simulation results are used to re-calibrate the fitting
parameters of the halofit model so as to reproduce small-scale power spectra of
the $N$-body simulations, while keeping the precision at large scales. The
revised fitting formula provides an accurate prediction of the nonlinear matter
power spectrum in a wide range of wavenumber ($k \leq 30h$\,Mpc$^{-1}$) at
redshifts $0 \leq z \leq 10$, with 5% precision for $k\leq1 h$ Mpc$^{-1}$ at $0
\leq z \leq 10$ and 10% for $1 \leq k\leq 10 h$ Mpc$^{-1} $ at $0 \leq z \leq
3$. We discuss the impact of the improved halofit model on weak lensing power
spectra and correlation functions, and show that the improved model better
reproduces ray-tracing simulation results.
