The dependence of the galaxy stellar-to-halo mass relation on galaxy
  morphology
  We 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
$10^{11.7}-10^{12.9}M_{\odot}$, 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 $10^{13}M_{\odot}$, discs are less massive than ellipticals in same-mass
haloes, regardless of whose stellar mass estimates we use. However, we find
that for these high halo masses the results for discs may be affected by
central/satellite misclassifications. The EAGLE simulation predicts that discs
are up to a factor of 1.5 more massive than elliptical galaxies residing in
same-mass haloes less massive than $10^{13}M_{\odot}$, in agreement with the
Kauffmann et al. data. Haloes with masses between $10^{11.5}$ and
$10^{12}M_{\odot}$, 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
$10^{12}-10^{12.5}M_{\odot}$ haloes, the central black holes in elliptical
galaxies grew faster and became 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.
