Bellagamba, FabioFabioBellagambaSereno, MauroMauroSerenoRONCARELLI, MauroMauroRONCARELLIMaturi, MatteoMatteoMaturiRADOVICH, MARIOMARIORADOVICHBARDELLI, SandroSandroBARDELLIPUDDU, Emanuella AnnaEmanuella AnnaPUDDUMOSCARDINI, LAUROLAUROMOSCARDINIGETMAN, FEDORFEDORGETMANHildebrandt, HendrikHendrikHildebrandtNAPOLITANO, NICOLA ROSARIONICOLA ROSARIONAPOLITANO2020-12-142020-12-1420190035-8711http://hdl.handle.net/20.500.12386/28825We present the mass calibration for galaxy clusters detected with the AMICO code in KiDS DR3 data. The cluster sample comprises 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 λ* (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 two-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<SUB>200</SUB> and the λ*-M<SUB>200</SUB> relations. The relations extend over more than 1 order of magnitude in mass, down to M_{200} ∼ 2 (5) × 10^{13} M_☉ h^{-1} at z = 0.2 (0.5), with small evolution in redshift. The logarithmic slope is 2.0 for the A-mass relation, and 1.7 for the λ*-mass relation, consistent with previous estimations on mock catalogues and coherent with the different nature of the two observables.STAMPAenArticle10.1093/mnras/stz0902-s2.0-85062427827000462302600013https://academic.oup.com/mnras/article/484/2/1598/52899022019MNRAS.484.1598BFIS/05 - ASTRONOMIA E ASTROFISICAERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_6 Stars and stellar systems