标题： EPOCHS 论文 V. 来自 JWST 观测的 z < 7 时星系形成对星系结构的依赖性 显示英文标题

标题： EPOCHS Paper V. The dependence of galaxy formation on galaxy structure at z < 7 from JWST observations

摘要： 我们通过研究基于 JWST CEERS 数据（来自扩展 Grot Strip，EGS）的星系在$z < 7$处的恒星质量所揭示的正在进行的恒星形成和综合恒星形成历史，来衡量星系结构对星系形成的整体影响。 利用 Ferreira 等人（2023）的 3965 个通过视觉分类的 JWST 星系形态目录，我们探讨了恒星的演化及其形成时间，这些都作为形态类型的函数以及通过光谱能量分布分类为被动和星爆星系的结果。 尽管盘状星系在$z < 7$的星系结构中占主导地位，但我们发现这些盘状星系通常要么是“被动”的，要么位于恒星形成的主序列上，并且不含大量星爆星系。 我们还发现，在$z < 7$处，形态类型与星系的恒星形成率或颜色之间没有显著的相关性。 事实上，我们发现形态分类为“椭圆星系”的星系倾向于呈现蓝色，并未被发现主要为被动系统在$z > 1.5$处。 我们还发现盘状星系的恒星质量函数在此期间并未显著演变，而其他星系类型，如奇特星系群体，则发生了戏剧性的变化，在较低红移处下降。 这表明在高红移处，巨大的奇特星系更为常见。 我们进一步发现，在$z \sim 7$处，特定恒星形成率（sSFR）不随视觉形态变化，但强烈依赖于恒星质量和星系内部的质量密度。 这表明在早期阶段，星系的组装过程是由质量驱动的，而不是由形态驱动的过程。 因此，恒星形成的熄灭在整个宇宙历史中是一个质量主导的过程，可能由于超大质量黑洞的存在所致。 显示英文摘要

摘要： We measure the broad impact of galaxy structure on galaxy formation by examining the ongoing star formation and integrated star formation history as revealed through the stellar masses of galaxies at $z < 7$ based on JWST CEERS data from the Extended Groth Strip (EGS). Using the morphological catalog of 3965 visually classified JWST galaxies from Ferreira et al. (2023), we investigate the evolution of stars, and when they form, as a function of morphological type as well as galaxies classified as passive and starburst through spectral energy distributions. Although disk galaxies dominate the structures of galaxies at $z < 7$, we find that these disks are in general either `passive', or on the main-sequence of star formation, and do not contain a large population of starburst galaxies. We also find no significant correlation between morphological type and the star formation rate or colours of galaxies at $z < 7$. In fact, we find that the morphologically classified `spheroids' tend to be blue and are not found to be predominately passive systems at $z > 1.5$. We also find that the stellar mass function for disk galaxies does not evolve significantly during this time, whereas other galaxy types, such as the peculiar population, evolve dramatically, declining at lower redshifts. This indicates that massive peculiars are more common at higher redshifts. We further find that up to $z \sim 7$, the specific star formation rate (sSFR) does not vary with visual morphology, but strongly depends on stellar mass and internal galaxy mass density. This demonstrates that at early epochs galaxy assembly is a mass-driven, rather than a morphologically-driven, process. Quenching of star formation is therefore a mass-dominated process throughout the universe's history, likely due to the presence of supermassive black holes.