The ALPINE-CRISTAL-JWST Survey: Gas-phase abundance gradients of main-sequence star-forming galaxies and their kinematics at 4<z<6

We present gas-phase radial metallicity profiles for /σ_0 increases towards later cosmic times, the observed negative trend with V_ main-sequence galaxies at 4<z<6 primarily based on JWST NIRSpec IFU observations obtained as part of the programme. Our study aims to connect the metallicity gradients of these galaxies with their kinematic properties from ̧ii,158 /σ_0 and the metallicity gradients, but no strong relationships with σ_0. As V_ ALMA observations. We mapped the radial profiles of oxygen abundance using the strong-line method, leveraging the rich set of rest-frame optical emission lines. Linear fits to the annular-binned radial profiles show that, on average, the metallicity gradients are slightly positive with a median of However, only three galaxies show a gradient $>$,0.05, /σ_0 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 σ_0 as well as the V_ ̊m rot ̊m rot ̊m rot ̊m rot /σ_0 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.