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We present an analysis of the quenching of star formation in massive galaxies($M_* > 10^{9.5} M_\odot$) within the first 0.5 - 3 Gyr of the Universe'shistory utilizing JWST-CEERS data. We utilize a combination of advancedstatistical methods to accurately constrain the intrinsic dependence ofquenching in a multi-dimensional and inter-correlated parameter space.Specifically, we apply Random Forest (RF) classification, area statistics, anda partial correlation analysis to the JWST-CEERS data. First, we identify thekey testable predictions from two state-of-the-art cosmological simulations(IllustrisTNG & EAGLE). Both simulations predict that quenching should beregulated by supermassive black hole mass in the early Universe. Furthermore,both simulations identify the stellar potential ($\phi_*$) as the optimal proxyfor black hole mass in photometric data. In photometric observations, where wehave no direct constraints on black hole masses, we find that the stellarpotential is the most predictive parameter of massive galaxy quenching at allepochs from $z = 0 - 8$, exactly as predicted by simulations for this sample.The stellar potential outperforms stellar mass, galaxy size, galaxy density,and S\'ersic index as a predictor of quiescence at all epochs probed inJWST-CEERS. Collectively, these results strongly imply a stable quenchingmechanism operating throughout cosmic history, which is closely connected tothe central gravitational potential in galaxies. This connection is explainedin cosmological models via massive black holes forming and growing in deeppotential wells, and subsequently quenching galaxies through a mix of ejectiveand preventative active galactic nucleus (AGN) feedback.

Galaxy quenching at the high redshift frontier: A fundamental test of cosmological models in the early universe with JWST-CEERS