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

## TL;DR

This study analyzes the metallicity and alpha-element abundances in the Milky Way bulge along its minor axis, revealing insights into its chemical evolution and differences from the disk and halo populations.

## Contribution

It provides new measurements of stellar parameters and chemical abundances along the bulge's minor axis using the HERMES spectrograph, comparing them with GALAH survey data.

## Key findings

- Metallicity components are closer by ~0.09 dex than previously thought.
- Alpha-element distribution varies with latitude, reflecting different stellar populations.
- Bulge shows rapid chemical evolution, distinct from the disk and halo.

## Abstract

To better understand the origin and evolution of the Milky Way bulge, we have conducted a survey of bulge red giant branch and clump stars using the HERMES spectrograph on the Anglo-Australian Telescope. We targeted ARGOS survey stars with pre-determined bulge memberships, covering the full metallicity distribution function. The spectra have signal-to-noise ratios comparable to, and were analysed using the same methods as the GALAH survey. In this work, we present the survey design, stellar parameters, distribution of metallicity and alpha-element abundances along the minor bulge axis at latitudes $b$ = $-10^{\circ}, -7.5^{\circ}$ and $-5^{\circ}$. Our analysis of ARGOS stars indicates 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 the different metallicity components. Closer to the plane, alpha abundance ratios are lower as the metal-rich population dominates. At higher latitudes, the alpha abundance ratios increase as the number of metal-poor stars increases. However, we find that the trend of alpha-enrichment with respect to metallicity is independent of latitude. Comparison of our results with those of GALAH DR2 revealed that for [Fe/H] $\approx -0.8$, the bulge shares the same abundance trend as the high-$\alpha$ disk population. However, the metal-poor bulge population ([Fe/H] $\lesssim -0.8$) show enhanced alpha abundance ratios compared to the disk/halo. These observations point to fairly rapid chemical evolution in the bulge, and that the metal-poor bulge population does not share the same similarity with the disk as the more metal-rich populations.