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There is a long-standing debate on the origin of the metal-poor stellarpopulations of the Milky Way (MW) bulge, with the two leading scenarios beingthat these populations are either i) part of a classical metal-poor spheroid orii) the same population as the chemically defined thick disc seen at the Solarneighbourhood. Here we test whether the latter scenario can reproduce theobserved chemical properties of the MW bulge. To do so we compare an N-bodysimulation of a composite (thin+thick) stellar disc -- which evolves secularlyto form a bar and a boxy/peanut (b/p) bulge -- to data from APOGEE DR13. Thismodel, in which the thick disc is massive and centrally concentrated, canreproduce the morphology of the metal-rich and metal-poor stellar populationsin the bulge, as well as the mean metallicity and [$\alpha$/Fe] maps asobtained from the APOGEE data. It also reproduces the trends, in both longitudeand latitude, of the bulge metallicity distribution function (MDF).Additionally, we show that the model predicts small but measurable azimuthalmetallicity variations in the inner disc due to the differential mapping of thethin and thick disc in the bar. We therefore see that the chemo-morphologicalrelations of stellar populations in the MW bulge are naturally reproduced bymapping the thin and thick discs of the inner MW into a b/p.

The disc origin of the Milky Way bulge: Dissecting the chemo-morphological relations using N-body simulations and APOGEE