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Fig. A.2.

image

Resulting f − M relation when varying the assumptions on the fit of the galaxy rotation curves. In the top row the dark matter halo model was varied: NFW (left), Burkert (centre), or Einasto (right). In the first two cases, the rotation curves were fit with a uniform prior on Υdisc, assuming Υbulge = 1.4Υdisc and with a prior on the concentration-mass relation for the NFW profile (from Dutton & Macciò 2014) and one on the core radius-core mass relation for the Burkert profile (from Salucci & Burkert 2000). Instead, the fits in the Einasto case were obtained by Ghari et al. (2019), who used the mass-to-light ratios derived by Li et al. (2018). In the bottom row, an NFW halo was used, but the assumptions on the mass-to-light ratios were varied: either fixed (left) or both left free to vary with the condition Υdisc ≤ Υbulge (right). In all panels the colouring of the points, the dashed horizontal line, and the abundance matching predictions (dashed curve with grey band) are as in Fig. 2.

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