Panel (a): Stellar masses of the entire MHUDF sample (with log(M_★/M_⊙) > 8.5) as a function of the offset from the SFMS (ΔMS) from Boogaard et al. (2018). The data points are colour-coded according to the DM inner slope, γ. The error bars show the 1σ statistical uncertainties in M_★ and SFR from Magphys. Panel (b): DM density at 150 pc as a function of log(M_★/M_vir). The data points are colour-coded according to their sSFRs. The error bars represent the 95% confidence intervals from our disk-halo decomposition. In both panels, the circles show the regular MHUDF galaxies, while the stars depict the perturbed systems from our sample. Panel (c): γ as a function of the stellar masses for the mass-matched MHUDF sample (red circles) and the TNG galaxies (black open squares, from Pillepich et al. 2019). The large indigo data points show the mean values for γ of the MHUDF sample in 6 mass bins, while the grey diamonds show the mean values for the mass-matched SPARC sample at z = 0 (using the DC14 fits without ΛCDM priors from Li et al. 2020). The green curve shows the predictions from Tollet et al. (2016) at z = 0, whereas the green shaded region shows the 0.18 dex scatter around the relation. The histogram shows the distribution of the γ values for the mass-matched MHUDF (in red), SPARC (in grey), TNG (in black), and NIHAO (in green) samples.