AMICO galaxy clusters in KiDS-DR3: weak-lensing mass calibration
  We present the mass calibration for galaxy clusters detected with the AMICO
code in KiDS DR3 data. The cluster sample comprises $\sim$ 7000 objects and
covers the redshift range 0.1 < $z$ < 0.6. We perform a weak lensing stacked
analysis by binning the clusters according to redshift and two different mass
proxies provided by AMICO, namely the amplitude $A$ (measure of galaxy
abundance through an optimal filter) and the richness $\lambda^*$ (sum of
membership probabilities in a consistent radial and magnitude range across
redshift). For each bin, we model the data as a truncated NFW profile plus a
2-halo term, taking into account uncertainties related to concentration and
miscentring. From the retrieved estimates of the mean halo masses, we construct
the $A$-$M_{200}$ and the $\lambda^*$-$M_{200}$ relations. The relations extend
over more than one order of magnitude in mass, down to $M_{200} \sim 2 (5)
\times 10^{13} M_\odot/h$ at $z$ = 0.2 (0.5), with small evolution in redshift.
The logarithmic slope is $\sim 2.0$ for the $A$-mass relation, and $\sim 1.7$
for the $\lambda^*$-mass relation, consistent with previous estimations on mock
catalogues and coherent with the different nature of the two observables.
