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We explore the radial distribution of star formation in galaxies in the SAMIGalaxy Survey as a function of their local group environment. Using a sample ofgalaxies in groups (with halo masses less than $ \simeq 10^{14} \,\mathrm{M_{\odot}}$) from the Galaxy And Mass Assembly Survey, we findsignatures of environmental quenching in high-mass groups ($M_{G} > 10^{12.5}\, \mathrm{M_{\odot}}$). The mean integrated specific star formation rate ofstar-forming galaxies in high-mass groups is lower than for galaxies inlow-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. Inhigh-mass groups, star-forming galaxies more massive than $M_{*} \sim 10^{10}\, \mathrm{M_{\odot}}$ have centrally-concentrated star formation. Thesegalaxies also lie below the star-formation main sequence, suggesting they maybe undergoing outside-in quenching. Lower mass galaxies in high-mass groups donot 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. Inthis regime we find a modest correlation between centrally-concentrated starformation and an enhancement in total star formation rate, consistent withtriggered star formation in these galaxies.

The SAMI Galaxy Survey: Observing the environmental quenching of star formation in GAMA groups