Measuring the scatter of the mass-richness relation in galaxy clusters
  in photometric imaging surveys by means of their correlation function
  Knowledge of the scatter in the mass-observable relation is a key ingredient
for a cosmological analysis based on galaxy clusters in a photometric survey.
In this paper we aim to quantify the capability of the correlation function of
galaxy cluster to constrain the intrinsic scatter $\sigma_{\ln M}$. We
demonstrate how the linear bias measured in the correlation function of
clusters can be used to determine the value of this parameter. The new method
is tested in simulations of a $5, 000 deg^2$ optical survey up to $z \sim 1$,
similar to the ongoing Dark Energy Survey (DES). Our results show that our
method works better at lower scatter values. We can measured the intrinsic
scatter $\sigma_{ln M} = 0.1$ with a standard deviation of $\sigma(\sigma_{ln
M}) \sim 0.03$ using this technique. However, the expected intrinsic scatter of
the DES RedMaPPer cluster catalog $\sigma_{ln M} \sim 0.2$ cannot be recovered
with this method at suitable accuracy and precision because the area coverage
is insufficient. For future photometric surveys with a larger area such as LSST
and Euclid, the statistical errors will be reduced. Therefore, we forecast
higher precision to measure the intrinsic scatter including the value mention
before. We conclude that this method can be used as an internal consistency
check method on their simplifying assumptions and complementary to
cross-calibration techniques in multi-wavelength cluster observations
