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Recent ALMA observations of the [OIII] 88 $\mu$m line provide spectroscopicconfirmation of two JWST photometric candidates, GS-z14 and GHZ2, at $z=14.2$and $z=12.3$, respectively. These discoveries reveal that star formation andchemical enrichment were already underway when the universe was merely 300 Myrold, posing a challenge to galaxy formation models. Here we constructpost-processed models for the [OIII] emission lines from galaxies in thestate-of-the-art FIRE and IllustrisTNG simulations. Neither simulation suitecontains galaxies directly comparable to GS-z14 or GHZ2. However, one simulatedFIRE galaxy closely resembles GS-z14 in its star formation rate (SFR), stellarmass, metallicity, [OIII] luminosity and line-width, albeit at $z=8.7$, laggingGS-z14's formation by roughly 300 Myr. Although further investigation isrequired, we argue that the lack of simulated galaxies matching GS-z14 and GHZ2may largely be a consequence of the limited volume of the FIRE simulations andthe limited mass resolution of Illustris-TNG. We quantify the prospects forfollow-up spectroscopic detections of GS-z14 in the [OIII] 52 $\mu$m line withALMA, and in rest-frame optical [OIII] and Balmer lines with the MIRIinstrument on JWST.

Do cosmological simulations reproduce the [OIII] 88 $\mu$m line emission and properties of JWST-discovered galaxies at $z \geq 12$?