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One of the best methods that we have for exploring the distribution of dark matter throughout the universe is to measure its gravitational influence on the observed shapes of background galaxies. On linear scales of ∼ 3 – 300 kpc, when the dark matter distribution is dominated by individual galaxy halos, the investigation is best performed statistically by correlating the orientations of the source...
We use a series of Monte Carlo simulations to investigate the theory of galaxy–galaxy lensing by non‐spherical dark matter haloes. The simulations include a careful accounting of the effects of multiple deflections on the galaxy–galaxy lensing signal. In a typical observational data set where the mean tangential shear of sources with redshifts zs≃ 0.6 is measured with respect to the observed symmetry...
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