Effects of varying the prior on the c − M_h correlation in our dynamical estimates of the SHMR. Top (bottom) panels: resulting f_⋆ − M_h (f_⋆ − M_⋆) relation, where the halo masses of both late types (blue diamonds) and early types (red circles) are calculated with a prior on the c − M_h relation that follows the purple shaded area (1σ) in the middle row of panels. From left to right: the four columns of panels are for the following priors: (i) the fiducial c − M_h relation from cosmological simulations by Dutton & Macciò (2014, with slope = −0.101 and scatter = 0.11 dex), (ii) the same c − M_h relation but with about twice the scatter (0.25 dex), (iii) a steeper one (slope = −0.2), and (iv) a shallower one (slope = −0.05). The black dashed lines in the middle panels show the fiducial c − M_h relation for comparison. Top and bottom rows: the grey shaded area shows the SHMR from Moster et al. (2013) based on abundance matching.