JWST Absorption-Line Analysis of UV-Bright Galaxies at $z=7.2-10.6$: Early Chemical Enrichment Traced by C, O, Mg, Al, Si, and Fe

We investigate UV absorption lines tracing cool gas in eight bright ($-21.9<M_{\mathrm{U}\mathrm{V}}<-20.5$) galaxies at $z=7.2-10.6$ using deep archival JWST/NIRSpec medium-resolution spectra. The eight galaxies were homogeneously selected based on wavelength coverage and data quality from 362 galaxies at $z>7$ available to date, and all eight were observed as part of the SPURS program. We identify multiple absorption lines of low-ionization species (LIS) in five galaxies, while the remaining three show only one or no significant detections. The average LIS equivalent widths (${\mathrm{E}\mathrm{W}}_{\mathrm{L}\mathrm{I}\mathrm{S}}$) indicate weaker absorption lines in compact ($r_{\mathrm{e}}\lesssim 100$ pc) galaxies with high $L_{\mathrm{H}\beta }\mathrm{/}{L}_{\mathrm{U}\mathrm{V}}$ and ${\mathrm{\Sigma }}_{\mathrm{S}\mathrm{F}\mathrm{R}}$, suggestive of absorption-line suppression due to intense star formation or nuclear activity. We simultaneously fit multiple LIS lines, accounting for both covering fraction ($C_f$) and column density ($N$), and find that the five galaxies follow the local $C_f$ versus $N$ relation. Through the LIS-line fitting, we derive chemical abundance ratios. The five galaxies have abundance ratios similar to those of damped Ly$\alpha$ (DLA) systems in the [Si/O] versus [C/O] and [Fe/Si] versus [Al/Si] planes, suggesting that their absorbing gas is similar to that of DLAs. We find that two galaxies at $z\sim 7$ are already highly Fe-enriched, with $[\mathrm{F}\mathrm{e}\mathrm{/}\mathrm{S}\mathrm{i}]\simeq -0.2$, near the solar abundance ratio. While the high Fe enrichment may originate from early Type-Ia supernovae (SNe Ia) or pair-instability supernovae (PISNe), these two galaxies also show $[\mathrm{A}\mathrm{l}\mathrm{/}\mathrm{S}\mathrm{i}]\sim 0$, with no signature of the strong odd-even effect expected from PISNe, favoring SNe Ia.