Schedule by Session

LSST and Euclid both promise significant advancements in the field of weak gravitational lensing cosmology. As such, it is crucial that relevant systematic effects such as the intrinsic alignment (IA) of galaxies are well-understood. Current methods for measuring IA may suffer from significant systematic errors in the context of future surveys, particularly due to uncertainty in the source galaxy redshift distribution. In an attempt to overcome this issue, I will describe a new method of measuring the scale-dependence of the IA signal, which takes advantage of information from multiple shape-measurement techniques. This procedure has the potential to reduce not only systematic error, but also statistical error, due to the fact that shape measurements from different methods will exhibit correlated noise.