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The merging history of galaxies can be traced with studies of dynamicallyclose pairs. These consist of a massive primary galaxy and a less massivesecondary (or satellite) galaxy. The study of the stellar populations ofsecondary (lower mass) galaxies in close pairs provides a way to understandgalaxy growth by mergers. Here we focus on systems involving at least onemassive galaxy - with stellar mass above $10^{11}M_\odot$ in the highlycomplete GAMA survey. Our working sample comprises 2,692 satellite galaxyspectra (0.1<z<0.3). These spectra are combined into high S/N stacks, andbinned according to both an "internal" parameter, the stellar mass of thesatellite galaxy (i.e. the secondary), and an "external" parameter, selectingeither the mass of the primary in the pair, or the mass of the correspondingdark matter halo. We find significant variations in the age of the populationswith respect to environment. At fixed mass, satellites around the most massivegalaxies are older and possibly more metal rich, with age differences ~1-2Gyrwithin the subset of lower mass satellites ($\sim 10^{10}M_\odot$). Thesevariations are similar when stacking with respect to the halo mass of the groupwhere the pair is embedded. The population trends in the lower-mass satellitesare consistent with the old stellar ages found in the outer regions of massivegalaxies.

Galaxy and Mass Assembly (GAMA): Probing the merger histories of massive galaxies via stellar populations