The origin of the enhanced metallicity of satellite galaxies

Observations of galaxies in the local Universe have shown that both the ionized gas and the stars of satellites are more metal-rich than of equally massive centrals. To gain insight into the connection between this metallicity enhancement and other differences between centrals and satellites, such as their star formation rates, gas content, and growth history, we study the metallicities of >3600 galaxies with M-star > 10(10) M-circle dot in the cosmological hydrodynamical EAGLE 100 Mpc 'Reference' simulation, including similar to 1500 in the vicinity of galaxy groups and clusters (M-200 >= 10(13)M(circle dot)). The simulation predicts excess gas and stellar metallicities in satellites consistent with observations, except for stellar metallicities at M-star less than or similar to 10(10.2)M(circle dot) where the predicted excess is smaller than observed. The exact magnitude of the effect depends on galaxy selection, aperture, and on whether the metallicity is weighted by stellar mass or luminosity. The stellar metallicity excess in clusters is also sensitive to the efficiency scaling of star formation feedback. We identify stripping of low-metallicity gas from the galaxy outskirts, as well as suppression of metal-poor inflows towards the galaxy centre, as key drivers of the enhancement of gas metallicity. Stellar metallicities in satellites are higher than in the field as a direct consequence of the more metal-rich star-forming gas, whereas stripping of stars and suppressed stellar mass growth, as well as differences in accreted versus in situ star formation between satellites and the field, are of secondary importance.