Main sequence relations at our two redshift slices. For our analysis we adopt the MS given by Eq. (9) (blue), but we also compare to MS relations with a shallower slope, (Speagle et al. 2014; green) and a MS relation with a turn-over at low redshifts and high stellar masses, Schreiber et al. (2015). The vertical dotted line at log (M_* ∕M_⊙) = 10.2 shows the mass cut used in this work. We note that the Speagle et al. (2014) and Schreiber et al. (2015) relations shown for comparison were not calibrated at z = 0.