Early Results from GLASS-JWST. IV. Spatially Resolved Metallicity in a Low-mass z 3 Galaxy with NIRISS

We report the first gas-phase metallicity map of a distant galaxy measured with the James Webb Space Telescope (JWST). We use the NIRISS slitless spectroscopy acquired by the GLASS Early Release Science program to spatially resolve the rest-frame optical nebular emission lines in a gravitationally lensed galaxy at z = 3.06 behind the A2744 galaxy cluster. This galaxy (dubbed GLASS-Zgrad1) has stellar mass ~10^8.6 M _⊙, instantaneous star formation rate ~8.6 M _⊙ yr^-1 (both corrected for lensing magnification), and global metallicity one-fourth solar. From its emission-line maps ([O III], Hβ, Hγ, [Ne III], and [O II]), we derive its spatial distribution of gas-phase metallicity using a well-established forward-modeling Bayesian inference method. The exquisite resolution and sensitivity of JWST/NIRISS, combined with lensing magnification, enable us to resolve this z ~ 3 dwarf galaxy in ≳50 resolution elements with sufficient signal, an analysis hitherto not possible. We find that the radial metallicity gradient of GLASS-Zgrad1 is strongly inverted (i.e., positive): ${\rm{\Delta }}\mathrm{log}({\rm{O}}/{\rm{H}})/{\rm{\Delta }}r$ = 0.165 ± 0.023 dex kpc^-1. This measurement is robust at $\gtrsim 4-\,\sigma $ confidence level against known systematics. This positive gradient may be due to tidal torques induced by a massive nearby (~15 kpc projected) galaxy, which can cause inflows of metal-poor gas into the central regions of GLASS-Zgrad1. These first results showcase the power of JWST wide-field slitless spectroscopic modes to resolve the mass assembly and chemical enrichment of low-mass galaxies in and beyond the peak epoch of cosmic star formation (z ≳ 2). Reaching masses ≲ 10⁹ M _⊙ at these redshifts is especially valuable to constrain the effects of galactic feedback and environment and is possible only with JWST's new capabilities. *Based on observations acquired by the JWST under the ERS program ID 1324 (PI T. Treu).