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Biviano Fig. 18. – This diagram indicates the clustercentric radius over which the listed mechanisms are effective in shaping galaxy properties. Two clusters are considered, with M200 masses ≃ 9 and ≃ 14 in units of 1014 M⊙ (Cl0024+17 and MS0451-03, respectively). Arrows indicate the cluster virial radii. The indicated tidal processes refer to interactions with the cluster potential, while the term “harassment” refers to the effect of galaxy-galaxy collisions. From [373]. A galaxy moving on a circular orbit in the core of a cluster with core radius rc will suffer tidal truncation of its external parts, beyond a radius [450] (20) rt ≈ rc σg .

These are galaxy properties that are unlikely to evolve . simultaneously (see Sect. 3 2) and orbital isotropization can be used as a clock for galaxy evolution in clusters. It is also important to determine the orbital characteristics of different cluster galaxy populations as a function of cluster mass and/or cluster structure, since orbital isotropization may occur at different epochs and proceed with different speeds depending on the global cluster properties. As a matter of fact, in some clusters ETGs and LTGs move with similar orbital anisotropies [242].

Dalcanton J. , ApJS, 137 (2001) 117 50 A. Biviano [69] Bartelmann M. , Clowe D. , et al. A. J. , Scaramella R. , Einasto J. , et al. , et al. L. , Buchert T. , et al. J. , ApJ, 591 (2003) 741 [86] Binney J. S. A. C. , Helv. Phys. N. S. , Mezzetti M. , et al. , et al. , Hoekstra H. , et al. -Z. , et al. H. , De Grandi S. , Tago E. P. A. Woudt, ASP Conf. , Romaniello M. , Sodre 111 ¨ hringer H. and Hasinger G. , Diaferio A. , et al. , et al. , et al. , et al. G. , Cappi A. , Katgert P. J. , Basilakos S.

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Galaxy Systems in the Optical and Infrared by A. Biviano


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