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To better understand the origin and evolution of the Milky Way bulge, we haveconducted a survey of bulge red giant branch and clump stars using the HERMESspectrograph on the Anglo-Australian Telescope. We targeted ARGOS survey starswith pre-determined bulge memberships, covering the full metallicitydistribution function. The spectra have signal-to-noise ratios comparable to,and were analysed using the same methods as the GALAH survey. In this work, wepresent the survey design, stellar parameters, distribution of metallicity andalpha-element abundances along the minor bulge axis at latitudes $b$ =$-10^{\circ}, -7.5^{\circ}$ and $-5^{\circ}$. Our analysis of ARGOS starsindicates that the centroids of ARGOS metallicity components should be located$\approx$0.09 dex closer together. The vertical distribution of$\alpha$-element abundances is consistent with the varying contributions of thedifferent metallicity components. Closer to the plane, alpha abundance ratiosare lower as the metal-rich population dominates. At higher latitudes, thealpha abundance ratios increase as the number of metal-poor stars increases.However, we find that the trend of alpha-enrichment with respect to metallicityis independent of latitude. Comparison of our results with those of GALAH DR2revealed that for [Fe/H] $\approx -0.8$, the bulge shares the same abundancetrend as the high-$\alpha$ disk population. However, the metal-poor bulgepopulation ([Fe/H] $\lesssim -0.8$) show enhanced alpha abundance ratioscompared to the disk/halo. These observations point to fairly rapid chemicalevolution in the bulge, and that the metal-poor bulge population does not sharethe same similarity with the disk as the more metal-rich populations.

HERBS I: Metallicity and alpha enhancement along the Galactic bulge minor axis