The Heavy Metal Survey: The Evolution of Stellar Metallicities, Abundance Ratios, and Ages of Massive Quiescent Galaxies Since z~2

We present the elemental abundances and ages of 19 massive quiescent galaxies at $z\sim 1.4$ and $z\sim 2.1$ from the Keck Heavy Metal Survey. The ultra-deep LRIS and MOSFIRE spectra were modeled using a full-spectrum stellar population fitting code with variable abundance patterns. The galaxies have iron abundances between [Fe/H] = -0.5 and -0.1 dex, with typical values of $-0.2$ [$-0.3$] at $z\sim 1.4$ [$z\sim 2.1$]. We also find a tentative $\log {\sigma }_v$-[Fe/H] relation at $z\sim 1.4$. The magnesium-to-iron ratios span [Mg/Fe]$=0.1$,–,$0.6$ dex, with typical values of $0.3$ [$0.5$] dex at $z\sim 1.4$ [$z\sim 2.1$]. The ages imply formation redshifts of $z_{\mathrm{f}\mathrm{o}\mathrm{r}\mathrm{m}}=2-8$. Compared to quiescent galaxies at lower redshifts, we find [Fe/H] was $\sim 0.2$ dex lower at $z=1.4-2.1$. We find no evolution in [Mg/Fe] out to $z\sim 1.4$, though the $z\sim 2.1$ galaxies are $0.2$ dex enhanced compared to $z=0-0.7$. A comparison of these results to a chemical evolution model indicates that galaxies at higher redshift form at progressively earlier epochs and over shorter star-formation timescales, with the $z\sim 2.1$ galaxies forming the bulk of their stars over 150 Myr at $z_{\mathrm{f}\mathrm{o}\mathrm{r}\mathrm{m}}\sim 4$. This evolution cannot be solely attributed to an increased number of quiescent galaxies at later times; several Heavy Metal galaxies have extreme chemical properties not found in massive galaxies at $z\sim 0.0-0.7$. Thus, the chemical properties of individual galaxies must evolve over time. Minor mergers also cannot fully account for this evolution as they cannot increase [Fe/H], particularly in galaxy centers. Consequently, the build-up of massive quiescent galaxies since $z\sim 2.1$ may require further mechanisms such as major mergers and/or central star formation.