  We study the environment in which a galaxy lies (i.e. field or group) and its
connection with the morphology of the galaxy. This is done by examining the
distribution of parametric and non-parametric statistics across the
star-formation rate (SFR) - stellar mass (M$_{\star}$) plane and studying how
these distributions change with the environment in the local universe
($z<0.15$).
  We determine the concentration (C), Gini, M$_{20}$, asymmetry, Gini-M$_{20}$
bulge statistic (GMB), 50\% light radius ($r_{50}$), total S\'{e}rsic index,
and bulge S\'{e}rsic index ($n_{Bulge}$) for galaxies from the Galaxy and Mass
Assembly (GAMA) survey using optical images from the Kilo Degree Survey. We
determine the galaxy environment using the GAMA group catalogue and split the
galaxies into field or group galaxies. The group galaxies are further divided
by the group halo mass (M$_{h}$) -
$11\leq\mathrm{log(M}_{h}/\mathrm{M}_\odot)<12$,
$12\leq\mathrm{log(M}_{h}/\mathrm{M}_\odot)<13$, and
$13\leq\mathrm{log(M}_{h}/\mathrm{M}_\odot)<14$ - and into central and
satellite galaxies. The galaxies in each of these samples are then placed onto
the SFR-M$_{\star}$ plane, and each parameter is used as a third dimension. We
fit the resulting distributions for each parameter in each sample using two
two-dimensional Gaussian distributions: one for star-forming galaxies and one
for quiescent galaxies. The coefficients of these Gaussian fits are then
compared between environments.
  Using C and $r_{50}$, we find that galaxies typically become larger as the
group mass increases. This change is greater for larger galaxies. There is no
indication that galaxies are typically more or less clumpy as the environment
changes. Using GMB and $n_{Bulge}$, we see that the star-forming galaxies do
not become more bulge or disk dominated as the group mass changes. Asymmetry
does not appear to be greatly influenced by environment.

Astrophysics of Galaxies