Fig. 6.
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Posterior predicted distribution in the lensing-only power-law slope, as a function of stellar mass density. Simulated values of γPL have been obtained from Equation (31). The two sets of contours correspond to the posteriors obtained by fitting models with a fixed value of ϵ, as indicated in the legend. Error bars are measurements from Shajib et al. (2021), Etherington et al. (2022), Tan et al. (2024).
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