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Fig. 7


Bias parameter measured in dynamically old (red), young (blue) and all (black) clusters. The dashed and dotted lines show the marginalised posterior probability distributions for dynamical states differentiated by the fraction of red galaxies or by the magnitude gap of two brightest galaxies, respectively. Dynamically old clusters tend to have deeper gravitational potential well (larger bias parameter) than dynamically young clusters with the same halo masses.

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