Many quiescent galaxies discovered in the early Universe by JWST raise fundamental questions on when and how these galaxies became and stayed quenched. Making use of the latest version of the semianalytic model GAEA that provides good agreement with the observed quenched fractions up to z ∼ 3, we make predictions for the expected fractions of quiescent galaxies up to z ∼ 7 and analyze the main quenching mechanism. We find that in a simulated box of 685 Mpc on a side, the first quenched massive (M⋆ ∼ 1011M⊙), Milky Way–mass, and low-mass (M⋆ ∼ 109.5M⊙) galaxies appear at z ∼ 4.5, z ∼ 6.2, and before z = 7, respectively. Most quenched galaxies identified at early redshifts remain quenched for more than 1 Gyr. Independently of galaxy stellar mass, the dominant quenching mechanism at high redshift is accretion disk feedback (quasar winds) from a central massive black hole, which is triggered by mergers in massive and Milky Way–mass galaxies and by disk instabilities in low-mass galaxies. Environmental stripping becomes increasingly more important at lower redshift.

中文翻译：

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第一个猝灭星系：何时以及如何？

詹姆斯韦伯太空望远镜在早期宇宙中发现的许多静止星系提出了关于这些星系何时以及如何变得并保持熄灭的基本问题。利用最新版本的半解析模型 GAEA，它与观测到的 z ∼ 3 以内的猝灭分数具有良好的一致性，我们对 z ∼ 7 以内的静止星系的预期分数进行了预测，并分析了主要的猝灭机制。我们发现，在一侧685 Mpc的模拟盒子中，第一个淬灭的大质量（M⋆∼1011M⊙）、银河系质量和低质量（M⋆∼109.5M⊙）星系出现在z∼4.5处，分别为 z ∼ 6.2 和 z = 7 之前。大多数在早期红移时发现的猝灭星系在超过 1 Gyr 的时间内仍然处于猝灭状态。与星系恒星质量无关，高红移的主要猝灭机制是来自中心大质量黑洞的吸积盘反馈（类星体风），它是由大质量星系和银河系质量星系的合并以及低质量星系中的吸积盘不稳定性触发的。在红移较低时，环境剥离变得越来越重要。