In this work, Joop Schaye and myself investigate the dependence of the local galaxy stellar-to-halo mass relation (SHMR) on galaxy morphology. We use data from the Sloan Digital Sky Survey DR7 with morphological classifications from Galaxy Zoo, and compare with the EAGLE cosmological simulation. At fixed halo mass in the mass range 10^11.7 − 10^12.9 M⊙, the median stellar masses of SDSS disc galaxies are up to a factor of 1.4 higher than the median masses of their elliptical counterparts. However, when we switch from the stellar masses from Kauffmann et al. to those calculated by Chang et al. or Brinchmann et al., the median SHMR from discs and ellipticals coincide in this mass range. For halo masses larger than 1013 M⊙, discs are less massive than ellipticals in same-mass haloes, regardless of whose stellar mass estimates we use. The EAGLE simulation pre- dicts that discs are up to a factor of 1.5 more massive than elliptical galaxies residing in same-mass haloes less massive than 10^13 M⊙, in agreement with the Kauffmann et al. data. Haloes with masses between 10^11.5 and 10^12 M⊙, that host disc galaxies, were assembled earlier than those hosting ellipticals. This suggests that the discs are more massive because they had more time for gas accretion and star formation. In 10^12 −10^12.5 M⊙ haloes, the central black holes in elliptical galaxies grew faster and be- came more massive than their counterparts in disc galaxies. This suggests that in this halo mass range the ellipticals are less massive because AGN feedback ejected more of the halo’s gas reservoir, reducing star formation, and suppressing the (re)growth of stellar discs.