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Dark Matter and the Assembly History of Massive Galaxies and Clusters

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Figure

Figure 2.1: Top:10 per cent down to roughly 0.5 per cent ofs for an NFW profile, and ρ−2 is the corresponding density.The functional forms proposed by NFW and Moore et al
Fig. 8.— The inner slope of the dark matter density profile plot-α
Figure 2.4: Top:Fig. 2. Color image of two cluster lenses observed by HST2218 at z = 0.175 and Right panel - Cl0024+1654 at zparameters Ω Inner region of the lensing cluster MS2137, which exhibits prominent tangentialand radial arcs
Figure 1. Top: the average projected mass profile Σ(R) (filled squares) with Mean surface density profile derived from strong and weak lensing measurements in fourits statistical 1 uncertainty as a function of the projected radius R, which is
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