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We present a comprehensive study of the chemical properties of the stellarhaloes of Milky-Way mass galaxies, analysing the transition between the innerto the outer haloes. We find the transition radius between the relativedominance of the inner-halo and outer-halo stellar populations to be ~15-20 kpcfor most of our haloes, similar to that inferred for the Milky Way from recentobservations. While the number density of stars in the simulated inner-halopopulations decreases rapidly with distance, the outer-halo populationscontribute about 20-40 per cent in the fiducial solar neighborhood, inparticular at the lowest metallicities. We have determined [Fe/H] profiles forour simulated haloes; they exhibit flat or mild gradients, in the range[-0.002, -0.01 ] dex/kpc. The metallicity distribution functions exhibitdifferent features, reflecting the different assembly history of the individualstellar haloes. We find that stellar haloes formed with larger contributionsfrom massive subgalactic systems have steeper metallicity gradients. Verymetal-poor stars are mainly contributed to the halo systems by lower-masssatellites. There is a clear trend among the predicted metallicity distributionfunctions that a higher fraction of low-metallicity stars are found withincreasing radius. These properties are consistent with the range of behavioursobserved for stellar haloes of nearby galaxies.

Stellar haloes in Milky-Way mass galaxies: From the inner to the outer haloes