Faraday Rotation Measure due to the Intergalactic Magnetic Field II: the
  Cosmological Contribution
  We investigate the Faraday rotation measure (RM) due to the intergalactic
magnetic field (IGMF) through the cosmic web up to cosmological distances,
using a model IGMF based on turbulence dynamo in the large-scale structure of
the universe. By stacking the IGMF and gas density data up to redshift $z=5$
and taking account of the redshift distribution of polarized background radio
sources against which the RM is measured, we simulate the sky map of the RM.
The contribution from galaxy clusters is subtracted from the map, based on
several different criteria of X-ray brightness and temperature. Our findings
are as follows. The distribution of RM for radio sources of different redshifts
shows that the root-mean-square (rms) value increases with redshift and
saturates for $z \ga 1$. The saturated value is RM$_{\rm rms} \approx$ several
${\rm rad m^{-2}}$. The probability distribution function of $|{\rm RM}|$
follows the lognormal distribution. The power spectrum has a broad plateau over
the angular scale of $\sim 1 - 0.1^\circ$ with a peak around $\sim 0.15^\circ$.
The second-order structure function has a flat profile in the angular
separation of $\ga 0.2^\circ$. Our results could provide useful insights for
surveys to explore the IGMF with the Square Kilometer Array (SKA) and upcoming
SKA pathfinders.
