  We investigate the contentious issue of the presence, or lack thereof, of
satellites mass segregation in galaxy groups using the Galaxy And Mass Assembly
(GAMA) survey, the GALFORM semi-analytic and the EAGLE cosmological
hydrodynamical simulation catalogues of galaxy groups. We select groups with
halo mass $12 \leqslant \log(M_{\text{halo}}/h^{-1}M_\odot) <14.5$ and redshift
$z \leqslant 0.32$ and probe the radial distribution of stellar mass out to
twice the group virial radius. All the samples are carefully constructed to be
complete in stellar mass at each redshift range and efforts are made to
regularise the analysis for all the data. Our study shows negligible mass
segregation in galaxy group environments with absolute gradients of
$\lesssim0.08$ dex and also shows a lack of any redshift evolution. Moreover,
we find that our results at least for the GAMA data are robust to different
halo mass and group centre estimates. Furthermore, the EAGLE data allows us to
probe much fainter luminosities ($r$-band magnitude of 22) as well as
investigate the three-dimensional spatial distribution with intrinsic halo
properties, beyond what the current observational data can offer. In both cases
we find that the fainter EAGLE data show a very mild spatial mass segregation
at $z \leqslant 0.22$, which is again not apparent at higher redshift.
Interestingly, our results are in contrast to some earlier findings using the
Sloan Digital Sky Survey. We investigate the source of the disagreement and
suggest that subtle differences between the group finding algorithms could be
the root cause.
