We study a sample of \sim 10 ^ { 4 } galaxy clusters in the redshift range 0.2 < z < 0.8 with masses M _ { 200 } > 5 \times 10 ^ { 13 } h _ { 70 } ^ { -1 } M _ { \odot } , discovered in the second Red-sequence Cluster Survey ( RCS2 ) .
The depth and excellent image quality of the RCS2 enabled us to detect the cluster-mass cross-correlation up to z \sim 0.7 .
To obtain cluster masses , concentrations , and halo biases , we fit a cluster halo model simultaneously to the lensing signal and to the projected density profile of red-sequence cluster members , because the latter provides tight constraints on the cluster miscentring distribution .
We parametrised the mass-richness relation as M _ { 200 } = A \times ( N _ { 200 } / 20 ) ^ { \alpha } and find A = ( 15.0 \pm 0.8 ) \times 10 ^ { 13 } h _ { 70 } ^ { -1 } M _ { \odot } and \alpha = 0.73 \pm 0.07 at low redshift ( 0.2 < z < 0.35 ) .
At intermediate redshift ( 0.35 < z < 0.55 ) , we find a higher normalisation , which points towards a fractional increase in the richness towards lower redshift caused by the build-up of the red sequence .
The miscentring distribution is well constrained .
Only \sim 30 % of our BCGs coincide with the peak of the dark matter distribution .
The distribution of the remaining BCGs are modelled with a 2D-Gaussian , whose width increases from 0.2 to 0.4 h _ { 70 } ^ { -1 } Mpc towards higher masses .
The ratio of width and r _ { 200 } is constant with mass and has an average value of 0.44 \pm 0.01 .
The mass-concentration and mass-bias relations agree fairly well with literature results at low redshift , but have a higher normalisation at higher redshifts , possibly because of selection and projection effects .
The concentration of the satellite distribution decreases with mass and is correlated to the concentration of the halo .