  We present observations of 18 galaxies from the Galaxy And Mass Assembly
(GAMA) survey made with the SPIRAL optical integral field unit (IFU) on the
Anglo-Australian Telescope. The galaxies are selected to have a narrow range in
stellar mass (6x10^9Msolar < M* <2x10^10 Msolar) in order to focus on the
effects of environment. Local galaxy environments are measured quantitatively
using 5th nearest neighbour surface densities. We find that the total star
formation rates (SFR) measured from the IFU data are consistent with total SFRs
measured from aperture correcting either GAMA or Sloan Digital Sky Survey
single-fibre observations. The mean differences are SFR_GAMA/SFR_IFU =
1.26+/-0.23, sigma=0.90 and for the Sloan Digital Sky Survey we similarly find
SFR_Brinchmann/SFR_IFU = 1.34+/-0.17, sigma=0.67. Examining the relationships
with environment, we find off-centre and clumpy Halpha emission is not
significantly dependent on environment, being present in 2/7 (29^+20_-11 per
cent) galaxies in high-density environments (>0.77 Mpc^-2), and 5/11
(45^+15_-13 per cent) galaxies in low-density environments (<0.77 Mpc^-2). We
find a weak but not significant relationship of the total star formation rates
of star-forming galaxies with environment. Due to the size of our sample and
the scatter observed we do not draw a definitive conclusion about a possible
SFR dependence on environment. Examining the spatial distribution of the Halpha
emission, we find no evidence for a change in shape or amplitude of the radial
profile of star-forming galaxies with environment. If these observations are
borne out in larger samples this would infer that any environment-driven
star-formation suppression must either act very rapidly (the
`infall-and-quench' model) or that galaxies must evolve in a density-dependent
manner (an `in-situ evolution' model).
