Cosmic shear without shape noise
  We describe a new method for reducing the shape noise in weak lensing
measurements by an order of magnitude. Our method relies on spectroscopic
measurements of disk galaxy rotation and makes use of the Tully-Fisher relation
in order to control for the intrinsic orientations of galaxy disks. For this
new proposed method, so-called Kinematic Lensing (KL), the shape noise ceases
to be an important source of statistical error. We use the CosmoLike software
package to simulate likelihood analyses for two Kinematic Lensing survey
concepts (roughly similar in scale to Dark Energy Survey Task Force Stage III
and Stage IV missions) and compare their constraining power to a cosmic shear
survey from the Large Synoptic Survey Telescope (LSST). Our forecasts in
seven-dimensional cosmological parameter space include statistical
uncertainties resulting from shape noise, cosmic variance, halo sample
variance, and higher-order moments of the density field. We marginalize over
systematic uncertainties arising from photometric redshift errors and shear
calibration biases considering both optimistic and conservative assumptions
about LSST systematic errors.
  We find that even the KL-Stage III is highly competitive with the optimistic
LSST scenario, while evading the most important sources of theoretical and
observational systematic error inherent in traditional weak lensing techniques.
Furthermore, the KL technique enables a narrow-bin cosmic shear tomography
approach to tightly constrain time-dependent signatures in the dark energy
phenomenon.
