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A merger can also form and/or activate a central black hole, hence an AGN, perhaps Galaxy systems in the optical and infrared 45 Fig. 20. 2. Starburst galaxies identified by their IR emission are indicated with filled dots. The triangle indicates an AGN. 5 Mpc are drawn around the central positions of A1763 and its neighbor A1770. Shaded regions highlight the kinematically-detected filaments, where most starburst galaxies are located [482]. with a certain delay after the starburst [471]. This is observationally supported by the fact that AGN host galaxies have colors and morphologies suggestive of a 1–4 Gyr old starburst associated with a merger event [472], and by the fact that a merger model fits the relation between fAGN and σv of galaxy systems [442].

The Galaxy systems in the optical and infrared 35 Fig. 13. – The MDR for z ∼ 1 clusters (circles with error bars from [312], dashed line from [313]) compared with the same relation in local clusters (solid line from [307, 314], dotted line from [308]). From [312]. 5 [329, 330, 331]. The CMR is rather tight in nearby clusters, but its mean color and scatter increase with clustercentric distance and decreasing local density [332, 333, 334, 335] and at the fainter end of the LF [336]. 5 Gyr from the cluster center to its outskirts [334].

It should be possible to rule out either the cuspy NFW or the cored Burkert with a ∼ 5 times larger data-set than the ones used so far. The currently loose constraints on the relation between mass and concentration can be made tighter, in order to confirm or reject the apparent (albeit marginal) discrepancy with the theoretical predictions [288, 235]. While constraints on the shape of c = c(M ) relation can only come by sampling the group mass scales, constraints on the normalization can also come by sampling the cluster mass scales alone, where kinematical methods are more powerful (because the number of available galaxies per cluster is larger).

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