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We analyse the structure and chemical enrichment of a Milky Way-like galaxywith a stellar mass of 2 10^{10} M_sun, formed in a cosmological hydrodynamicalsimulation. It is disk-dominated with a flat rotation curve, and has a diskscale length similar to the Milky Way's, but a velocity dispersion that is ~50%higher. Examining stars in narrow [Fe/H] and [\alpha/Fe] abundance ranges, wefind remarkable qualitative agreement between this simulation and observations:a) The old stars lie in a thickened distribution with a short scale length,while the young stars form a thinner disk, with scale lengths decreasing, as[Fe/H] increases. b) Consequently, there is a distinct outward metallicitygradient. c) Mono-abundance populations exist with a continuous distribution ofscale heights (from thin to thick). However, the simulated galaxy has adistinct and substantive very thick disk (h_z~1.5 kpc), not seen in the MilkyWay. The broad agreement between simulations and observations allows us to testthe validity of observational proxies used in the literature: we find in thesimulation that mono-abundance populations are good proxies for single agepopulations (<1 Gyr) for most abundances.

MaGICC Thick Disk I: Comparing a Simulated Disk Formed with Stellar Feedback to the Milky Way