Cosmology without cosmic variance
  We examine the improvements in constraints on the linear growth factor G and
its derivative f=d ln G / dln a that are available from the combination of a
large-scale galaxy redshift survey with a weak gravitational lensing survey of
background sources. In the linear perturbation theory limit, the
bias-modulation method of McDonald & Seljak allows one to distinguish the
real-space galaxy clustering from the peculiar velocity signal in each Fourier
mode. The ratio of lensing signal to galaxy clustering in transverse modes
yields the bias factor b of each galaxy subset (as per Pen 2004), hence
calibrating the conversion from galaxy real-space density to matter density in
every mode. In combination these techniques permit measure of the growth rate f
in each Fourier mode. This yields a measure of the growth rate free of sample
variance, i.e. the uncertainty in f can be reduced without bound by increasing
the number of redshifts within a finite volume. In practice, the gain from the
absence of sample variance is bounded by the limited range of bias modulation
among dark-matter halos. Nonetheless, the addition of background weak lensing
data to a redshift survey increases information on G and f by an amount
equivalent to a 10-fold increase in the volume of a standard redshift-space
distortion measurement---if the lensing signal can be measured to sub-percent
accuracy. This argues that a combined lensing and redshift survey over a common
low-redshift volume is a more powerful test of general relativity than an
isolated redshift survey over larger volume at high redshift. An example case
is that a survey of ~10^6 redshifts over half the sky in the redshift range
$z=0.5\pm 0.05$ can determine the growth exponent \gamma for the model
$f=\Omega_m^\gamma$ to an accuracy of $\pm 0.015$, using only modes with
k<0.1h/Mpc, but only if a weak lensing survey is conducted in concert.
[Abridged]
