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We present gas-phase elemental abundance ratios of 7 local extremelymetal-poor galaxies (EMPGs) including our new Keck/LRIS spectroscopydeterminations together with 33 JWST $z\sim 4-10$ star-forming galaxies in theliterature, and compare chemical evolution models. We develop chemicalevolution models with the yields of core-collapse supernovae (CCSNe), Type Iasupernovae, hypernovae (HNe), and pair-instability supernovae (PISNe), andcompare the EMPGs and high-$z$ galaxies in conjunction with dust depletioncontributions. We find that high Fe/O values of EMPGs can (cannot) be explainedby PISN metal enrichments (CCSN/HN enrichments even with themixing-and-fallback mechanism enhancing iron abundance), while that theobserved Ar/O and S/O values are much smaller than the predictions of the PISNmodels. The abundance ratios of the EMPGs can be explained by the combinationof Type Ia SNe and CCSNe/HNe whose inner layers of argon and sulfur mostlyfallback, which are comparable with Sculptor stellar chemical abundancedistribution, suggesting that early chemical enrichment is taken place in theEMPGs. Comparing our chemical evolution models with the star-forming galaxiesat $z\sim 4-10$, we find that the Ar/O and S/O ratios of the high-$z$ galaxiesare comparable with those of the CCSNe/HNe models, while majority of thehigh-$z$ galaxies do not have constraints good enough to rule out contributionsfrom PISNe. The high N/O ratio recently reported in GN-z11 cannot be explainedeven by rotating PISNe, but could be reproduced by the winds of rotating WolfRayet stars that end up as a direct collapse.

EMPRESS. XIII. Chemical Enrichments of Young Galaxies Near and Far at z  ~ 0 and 4-10: Fe/O, Ar/O, S/O, and N/O Measurements with Chemical Evolution  Model Comparisons