Equivalent width distribution of Mg II absorbers in clusters (corrected by the cluster redshift path) vs. Mg II λ2796 rEW for LOS‐cluster distances ﹩d< 2﹩ ﹩h^{-1}_{71}﹩ Mpc (left) and ﹩d< 1﹩ ﹩h^{-1}_{71}﹩ Mpc (right). The error bars correspond to 1 σ. Data points with ﹩W_{0}< 1.0﹩ Å resulted from sample S1 only (high‐resolution spectra), while points at ﹩W_{0}> 1.0﹩ Å resulted from sample S2. The lines are the field expectations. The solid line is the exponential distribution fitted by NTR06 to their MMT data having ﹩W_{0}> 0.3﹩ Å, and the dashed line is the power law fitted by C99 to their HIRES data having ﹩W_{0}< 0.3﹩ Å. The vertical line at ﹩W_{0}=0.3﹩ Å marks the transition in ﹩n( W) ﹩ pointed out by NTR06.