  We explore the radial distribution of star formation in galaxies in the SAMI
Galaxy Survey as a function of their local group environment. Using a sample of
galaxies in groups (with halo masses less than $ \simeq 10^{14} \,
\mathrm{M_{\odot}}$) from the Galaxy And Mass Assembly Survey, we find
signatures of environmental quenching in high-mass groups ($M_{G} > 10^{12.5}
\, \mathrm{M_{\odot}}$). The mean integrated specific star formation rate of
star-forming galaxies in high-mass groups is lower than for galaxies in
low-mass groups or that are ungrouped, with $\Delta \log(sSFR/\mathrm{yr^{-1}})
= 0.45 \pm 0.07$. This difference is seen at all galaxy stellar masses. In
high-mass groups, star-forming galaxies more massive than $M_{*} \sim 10^{10}
\, \mathrm{M_{\odot}}$ have centrally-concentrated star formation. These
galaxies also lie below the star-formation main sequence, suggesting they may
be undergoing outside-in quenching. Lower mass galaxies in high-mass groups do
not show evidence of concentrated star formation. In groups less massive than
$M_{G} = 10^{12.5} \, \mathrm{M_{\odot}}$ we do not observe these trends. In
this regime we find a modest correlation between centrally-concentrated star
formation and an enhancement in total star formation rate, consistent with
triggered star formation in these galaxies.
