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We use a complete sample of 38 richest maxBCG clusters to study theICM-galaxy scaling relations and the halo mass selection properties of themaxBCG algorithm, based on X-ray and optical observations. The clusters areselected from the two largest bins of optical richness in the Planck stackingwork with the maxBCG richness $N_{200} \geq 78$. We analyze their Chandra andXMM-Newton data to derive the X-ray properties of the ICM. We then use thedistribution of $P(X|N)$, $X=T_X,\ L_X,\ Y_X$, to study the mass selection$P(M|N)$ of maxBCG. Compared with previous works based on the whole richnesssample, a significant fraction of blended systems with boosted richness isskewed into this richest sample. Parts of the blended halos are picked apart bythe redMaPPer, an updated red-sequence cluster finding algorithm with lowermass scatter. Moreover, all the optical blended halos are resolved asindividual X-ray halos, following the established $L_X-T_X$ and $L_X-Y_X$relations. We further discuss that the discrepancy between ICM-galaxy scalingrelations, especially for future blind stacking, can come from several factors,including miscentering, projection, contamination of low mass systems, massbias and covariance bias. We also evaluate the fractions of relaxed and coolcore clusters in our sample. Both are smaller than those from SZ or X-rayselected samples. Moreover, disturbed clusters show a higher level of mass biasthan relaxed clusters.

X-ray scaling relations from a complete sample of the richest maxBCG clusters