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Fig. A.1.

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Estimated Einstein radius of a power-law lens with θE = 1″, as a function of density slope and orbital anisotropy. The lens is at zg = 0.2, with a half-light radius Re = 7 kpc, and the Einstein radius is computed with respect to a source at zs = 0.6. White lines connect points of constant θ E ( est ) $ \theta_{\mathrm{E}}^{(\mathrm{est})} $. These are also points of constant velocity dispersion. In general, θ E ( est ) < θ E $ \theta_{\mathrm{E}}^{(\mathrm{est})} < \theta_{\mathrm{E}} $: this is because the line-of-sight velocity dispersion, which is used to estimate θ E ( est ) $ \theta_{\mathrm{E}}^{(\mathrm{est})} $, is smaller than the three-dimensional velocity dispersion of a singular isothermal sphere, due to projection effects.

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