发表机构
Terra Nova Sciences LLC; Johns Hopkins University（特拉诺瓦科学有限责任公司; 约翰斯·霍普金斯大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究构建连接功率谱与晕质量函数的框架，对比ST与KST校准，通过三项检验约束JWST高红移大质量星系和AGN的宿主晕丰度，揭示群体一致性需宿主晕数量充足。
AI 中文摘要
詹姆斯·韦布空间望远镜（JWST）在高红移处发现的大质量星系和明亮的活动星系核（AGN）为宇宙学结构形成与使暗物质晕可观测的天体物理过程之间的联系提供了日益灵敏的检验。我们开发了一个框架，将线性物质功率谱与质量方差、峰高、暗物质晕质量函数（HMF）、累积晕丰度以及可观测的星系和AGN群体联系起来。我们以Sheth-Tormen（ST）HMF为基线，并将其与一个示例性的Bolshoi-Klypin校准修正（KST）进行比较，以量化预测对HMF相对于宇宙学N体模拟校准的敏感性。我们将该框架应用于三项互补检验：大质量星系可用的重子和恒星质量储备、能够承载明亮AGN的暗物质晕丰度，以及高红移星系的静止系紫外光度函数。由于最大质量的系统占据晕分布的稀有高峰尾部，推断的宿主质量、重子转换效率、黑洞占据率或占空比以及HMF校准的适度变化可导致预测丰度的大幅变化。ST-KST比较表明，高红移晕群体的不确定性可实质性影响推断的宿主供给，尤其是在z（10）较大时。与代表性JWST大质量星系、AGN和紫外光度函数测量的比较表明，匹配单个源的性质不足以实现群体一致性；相应的宿主晕也必须以足够的数量存在。当前观测为宇宙学晕丰度以及宇宙黎明时的重子和黑洞物理提供了日益严格的定量压力测试。
英文摘要
The discovery by the James Webb Space Telescope (JWST) of massive galaxies and luminous active galactic nuclei (AGN) at high redshift provides an increasingly sensitive test of the connection between cosmological structure formation and the astrophysical processes that make dark matter halos observable. We develop a framework connecting the linear matter power spectrum to the mass variance, peak height, halo mass function (HMF), cumulative halo abundance, and observable galaxy and AGN populations. We use the Sheth-Tormen (ST) HMF as the baseline and compare it with an illustrative Bolshoi-Klypin-calibrated modification (KST) to quantify the sensitivity of predictions to the calibration of the HMF against cosmological N-body simulations. We apply the framework to three complementary tests: the baryonic and stellar mass reservoir available to massive galaxies, the abundance of halos capable of hosting luminous AGN, and the rest frame ultraviolet luminosity function of high redshift galaxies. Because the most massive systems occupy the rare, high peak tail of the halo distribution, modest changes in inferred host mass, baryonic conversion efficiency, black-hole occupation or duty cycle, and HMF calibration can produce large changes in predicted abundances. The ST-KST comparison shows that uncertainty in the high redshift halo population can materially affect the inferred host supply, particularly toward large z (10). Comparison with representative JWST massive galaxy, AGN, and UV luminosity function measurements demonstrates that matching the properties of an individual source is not sufficient for population consistency; the corresponding host halos must also exist in adequate numbers. Current observations provide increasingly stringent quantitative stress tests of both cosmological halo abundances and the baryonic and black hole physics at cosmic dawn.
Comments35 pages, 11 figures
