原初黑洞宇宙中的卫星恒星-暗物质晕质量关系
Satellite stellar-to-halo mass relations in primordial black hole universes
- CONICET（阿根廷国家科学研究委员会）
- Instituto de Astronomía Teórica y Experimental (IATE)（理论与实验天体物理研究所）
- Universidad Nacional de Córdoba (UNC)（科尔多瓦国立大学）
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
本研究通过对比CDM与FCT/PBH模拟，发现原初黑洞增强次暗晕丰度并使其更致密，但卫星恒星质量函数判别力弱，内部结构和动力学是更强检验，卫星丰度、动力学与致密暗扰子互为补充探针。
AI中文摘要：
原初黑洞（PBH），特别是具有固定共形时间（FCT）扩展质量函数的原初黑洞，可以通过增强的原初功率和离散性驱动的泊松涨落来改变小尺度结构，从而改变次暗晕的丰度和内部结构。我们研究了它们对卫星恒星-暗物质晕映射、束缚残骸致密性以及与致密暗扰子联系的影响。我们比较了两个仅含暗物质的模拟：一个基准的CDM模拟和一个FCT/PBH模拟。由于这些模拟不形成星系，我们利用最后孤立时的前身晕维里质量构建了一个近似的基于丰度的恒星-暗物质晕映射。CDM映射锚定于一个随红移变化的丰度匹配恒星-暗物质晕关系，而FCT映射则基于相对累积次暗晕丰度推导得出。我们使用解析的SOAP（V_max）和（R_max）来表征当前次暗晕的致密性，并辅以对未解析PBH种群中质量分层的亚网格估计。FCT以依赖于质量的方式增强了次暗晕丰度，但基于丰度的恒星质量重新分配使得卫星恒星质量函数成为较弱的判别量。内部结构是更强的检验：FCT次暗晕更致密，在固定半径处具有更大的NFW重建包围质量，如果所有致密次暗晕都承载发光卫星，则会加剧类似“太大而无法失败”的张力。FCT次暗晕也形成得更早，这解释了低质量致密性差异的大部分，而PBH质量分层则增加了典型的μ~0.4-0.5的中心扰动。这两种效应都不能完全解释解析的FCT致密性增强。星系-暗物质晕映射的变化可以部分隐藏卫星计数中增强的FCT次暗晕丰度，而内部动力学仍然更具区分性。卫星丰度、动力学和致密暗扰子是PBH诱导的小尺度结构的互补探针。
英文摘要：
Primordial black holes (PBHs), in particular with a fixed-conformal-time (FCT) extended mass function, can modify small-scale structure through enhanced primordial power and discreteness-driven Poisson fluctuations, altering subhalo abundances and internal structure. We study their effects on satellite stellar-to-halo mappings, bound-remnant compactness, and the link to compact dark perturbers. We compare two dark-matter-only simulations, a fiducial CDM run and an FCT/PBH run. As these runs form no galaxies, we construct an approximate abundance-based stellar-to-halo mapping using the progenitor virial mass at last isolation. The CDM mapping is anchored to a redshift-dependent abundance-matching stellar-to-halo relation, and the FCT mapping is derived from the relative cumulative subhalo abundances. We use resolved SOAP (V_max) and (R_max) to characterize present-day subhalo compactness, supplemented by a subgrid estimate of mass segregation in the unresolved PBH population. FCT enhances the subhalo abundance in a mass-dependent way, but abundance-based stellar-mass reassignment makes satellite stellar-mass functions weak discriminants. Internal structure is a stronger test: FCT subhaloes are more compact and have larger NFW-reconstructed enclosed masses at fixed radius, strengthening a Too-Big-To-Fail-like tension if all compact subhaloes host luminous satellites. FCT subhaloes also form earlier, accounting for much of the low-mass compactness difference, while PBH mass segregation adds a central perturbation with typical μ~ 0.4-0.5. Neither effect fully explains the resolved FCT compactness enhancement. Changes in the galaxy--halo mapping can partly hide the enhanced FCT subhalo abundance in satellite counts, whereas internal dynamics remain more discriminating. Satellite abundances, dynamics, and compact dark perturbers are complementary probes of PBH-induced small-scale structure.
