Prospects for Determining the Mass Distributions of Galaxy Clusters on
  Large Scales Using Weak Gravitational Lensing
  For more than two decades, the Navarro, Frenk, and White (NFW) model has
stood the test of time; it has been used to describe the distribution of mass
in galaxy clusters out to their outskirts. Stacked weak lensing measurements of
clusters are now revealing the distribution of mass out to and beyond their
virial radii, where the NFW model is no longer applicable. In this study we
assess how well the parameterised Diemer & Kravstov (DK) density profile
describes the characteristic mass distribution of galaxy clusters extracted
from cosmological simulations. This is determined from stacked synthetic
lensing measurements of the 50 most massive clusters extracted from the
Cosmo-OWLS simulations, using the Dark Matter Only run and also the run that
most closely matches observations. The characteristics of the data reflect the
Weighing the Giants survey and data from the future Large Synoptic Survey
Telescope (LSST). In comparison with the NFW model, the DK model favored by the
stacked data, in particular for the future LSST data, where the number density
of background galaxies is higher. The DK profile depends on the accretion
history of clusters which is specified in the current study. Eventually however
subsamples of galaxy clusters with qualities indicative of disparate accretion
histories could be studied.
