Next Generation Virgo Cluster Survey. XXI. The weak lensing masses of
  the CFHTLS and NGVS RedGOLD galaxy clusters and calibration of the optical
  richness
  We measured stacked weak lensing cluster masses for a sample of 1325 galaxy
clusters detected by the RedGOLD algorithm in the Canada-France-Hawaii
Telescope Legacy Survey W1 and the Next Generation Virgo Cluster Survey at
$0.2<z<0.5$, in the optical richness range $10<\lambda<70$. After a selection
of our best richness subsample ($20<\lambda<50$), this is the most
comprehensive lensing study of a $\sim 100\%$ complete and $\sim 90\%$ pure
optical cluster catalogue in this redshift range, with a total of 346 clusters
in $\sim164~deg^2$. We test three different mass models, and our best model
includes a basic halo model, with a Navarro Frenk and White profile, and
correction terms that take into account cluster miscentering, non-weak shear,
the two-halo term, the contribution of the Brightest Cluster Galaxy, and an a
posteriori correction for the intrinsic scatter in the mass-richness relation.
With this model, we obtain a mass-richness relation of $\log{M_{\rm
200}/M_{\odot}}=(14.48\pm0.04)+(1.14\pm0.23)\log{(\lambda/40)}$ (statistical
uncertainties). This result is consistent with other published lensing
mass-richness relations. When compared to X-ray masses and mass proxies, we
find that on average weak lensing masses are $\sim 10\%$ higher than those
derived in the X-ray in the range $2\times10^{13}M_{\rm \odot}<E(z) M^{X}_{\rm
200}<2\times10^{14}M_{\rm \odot}$, in agreement with most previous results and
simulations. We also give the coefficients of the scaling relations between the
lensing mass and X-ray mass proxies, $L_X$ and $T_X$, and compare them with
previous results.
