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We present a study of the relationships and environmental dependenciesbetween stellar mass, star formation rate, and gas metallicity for more than700 galaxies in groups up to redshift 0.35 from the Galaxy And Mass Assembly(GAMA) survey. To identify the main drivers, our sample was analyzed as afunction of group-centric distance, projected galaxy number density, andstellar mass. By using control samples of more than 16000 star-forming fieldgalaxies and volume limited samples, we find that the highest enhancement inSFR (0.3 dex) occurs in galaxies with the lowest local density. In contrast toprevious work, our data show small enhancements of $\sim$0.1 dex in SFR forgalaxies at the highest local densities or group-centric distances. Our dataindicates quenching in SFR only for massive galaxies, suggesting that stellarmass might be the main driver of quenching processes for star forming galaxies.We can discard a morphological driven quenching, since the S\'ersic indexdistribution for group and control galaxies are similar. The gas metallicitydoes not vary drastically. It increases $\sim$0.08 dex for galaxies at thehighest local densities, and decreases for galaxies at the highestgroup-centric distances, in agreement with previous work. Altogether, the localdensity, rather than group-centric distance, shows the stronger impact inenhancing both, the SFR and gas metallicity. We applied the same methodology togalaxies from the IllustrisTNG simulations, and although we were able toreproduce the general observational trends, the differences between group andcontrol samples only partially agree with the observations

Galaxy And Mass Assembly (GAMA): The environmental impact on SFR and metallicity in galaxy groups