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Fig. B.1

image

Results from fitting an NFW (top panel) and DC14 (bottom panel) to the outer-most point of the rotation curves of the observations used in Papastergis & Shankar (2016) using a fixed halo mass, keeping the halo concentration as a free parameter. The halo mass is calculated from their stellar mass using the abundance-matching relation of Moster et al. (2013). Red and blue lines and bands are the same as in Fig. 8.

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