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Near-field observations may provide tight constraints - i.e. "boundaryconditions" - on any model of structure formation in the Universe. Detailedobservational data have long been available for the Milky Way (e.g. Freeman$\&$ Bland-Hawthorn 2002) and have provided tight constraints on several Galaxyformation models (e.g. Abadi et al. 2003, Bekki $\&$ Chiba 2001). An implicitassumption still remains unanswered though: is the Milky Way a "normal" spiral?Searching for directions, it feels natural to look at our neighbour: Andromeda.An intriguing piece of the puzzle is provided by contrasting its stellar halowith that of our Galaxy, even more so since Mouhcine et al. (2005) havesuggested that a correlation between stellar halo metallicity and galacticluminosity is in place and would leave the Milky Way halo as an outlier withrespect to other spirals of comparable luminosities. Further questions hencearise: is there any stellar halo-galaxy formation symbiosis? Our first step hasbeen to contrast the chemical evolution of the Milky Way with that of Andromedaby means of a semi-analytic model. We have then pursued a complementaryapproach through the analysis of several semi-cosmological late-type galaxysimulations which sample a wide variety of merging histories. We have focusedon the stellar halo properties in the simulations at redshift zero and shownthat - at any given galaxy luminosity - the metallicities of the stellar halosin the simulations span a range in excess of $\sim$ 1 dex, a result which isstrengthened by the robustness tests we have performed. We suggest that theunderlying driver of the halo metallicity dispersion can be traced to thediversity of galactic mass assembly histories inherent within the hierarchicalclustering paradigm.

The Formation of Stellar Halos in Late-Type Galaxies