We present gas-phase radial metallicity profiles for /σ₀ increases towards later cosmic times, the observed negative trend with V_ main-sequence galaxies at 4, 0. 05, /σ₀ ratio of the disks. Combining our sample with mass-matched literature samples at 3łesssim złesssim7, we found a negative shallow correlation between V_ at 1σ, and none have a significant negative gradient. There are no substantial systematic offsets in gradients when using different line diagnostics. We investigated the correlation between the metallicity gradients and the intrinsic gas velocity dispersion σ₀ as well as the V_ ̊m rot ̊m rot ̊m rot ̊m rot /σ₀ is consistent with the overall cosmic evolution of metallicity gradients from high to low redshifts. This suggests that disk maturity plays a crucial role in shaping the radial metallicity gradients. We do not find the metallicity gradients of disk galaxies to be significantly different from non-disk galaxies, which could be attributed to the frequent accretion events that took place in these gas-rich systems. Additionally, we find no strong dependence of metallicity gradients on stellar mass and only a marginal positive dependence on specific star-formation rate. Our study extends the efforts to connect the internal kinematics of galaxies with their gas-phase chemical enrichment at kiloparsec scales from cosmic noon to z, >, 4.
Lee et al. (Wed,) studied this question.