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Concentration is one of the key dark matter halo properties that could drivethe scatter in the stellar-to-halo mass relation of massive clusters. We deriverobust photometric stellar masses for a sample of brightest central galaxies(BCGs) in SDSS redMaPPer clusters at $0.17<z<0.3$, and split the clusters intotwo equal-halo mass subsamples by their BCG stellar mass $M_*$. The weaklensing profiles $\Delta\Sigma$ of the two cluster subsamples exhibit differentslopes on scales below 1 M$pc/h$. To interpret such discrepancy, we perform acomprehensive Bayesian modelling of the two $\Delta\Sigma$ profiles byincluding different levels of miscentring effects between the two subsamples asinformed by X-ray observations. We find that the two subsamples have the sameaverage halo mass of $1.74 \times 10^{14} M_{\odot}/h$, but the concentrationof the low-$M_*$ clusters is $5.87_{-0.60}^{+0.77}$, ${\sim}1.5\sigma$ smallerthan that of their high-$M_*$ counterparts~($6.95_{-0.66}^{+0.78}$).Furthermore, both cluster weak lensing and cluster-galaxy cross-correlationsindicate that the large-scale bias of the low-$M_*$, low-concentration clustersare ${\sim}10\%$ higher than that of the high-$M_*$, high-concentrationsystems, hence possible evidence of the cluster assembly bias effect. Ourresults reveal a remarkable physical connection between the stellar mass within20{-}30 k$pc/h$, the dark matter mass within ${\sim}$ 200 k$pc/h$, and thecosmic overdensity on scales above 10 M$pc/h$, enabling a key observationaltest of theories of co-evolution between massive clusters and their centralgalaxies.

Does Concentration Drive the Scatter in the Stellar-to-Halo Mass Relation of Galaxy Clusters?