AI 中文总结
本文指出CMB功率谱并非唯一支持暗物质，米尔格罗姆引力模型也符合；并论证CMB谱是模型依赖的重建量，未扣除的河外前景（贡献≥1.4%）可能引入10^{-5}涨落。
AI 中文摘要
在热大爆炸图像中，按照标准LCDM框架及其椭圆星系层级并合情景的通常解释，宇宙微波背景（CMB）与红移z≈1100处的光子退耦相关，普朗克卫星的角功率谱被用来约束后来结构形成所依赖的10^{-5}量级的原初涨落。我们表明，除LCDM模型外，基于米尔格罗姆引力的两种宇宙学模型也与普朗克CMB功率谱一致，因此这些谱并不唯一支持暗物质的存在。我们进一步论证，已发表的CMB谱并非直接观测量，而是在扣除前景、并修正弱引力透镜、光子-电子散射以及视线方向引力能量红移后重建的量。由于这些步骤依赖于假定的结构增长历史，所得谱取决于数据处理中所采用的宇宙学模型。我们还注意到，已报道的CMB半球不对称性与椭圆星系在天球上超出预期的分布之间的相关性，可能指向跨越可观测宇宙大范围的非均匀物质分布。受椭圆星系层级并合中观测张力的启发，我们回顾了在降尺度时间尺度上椭圆星系形成的后果，这意味着在15< z <20期间释放了显著的河外前景。在保守假设下，该前景至少贡献了观测到的CMB能量密度的1.4%，且尚未被纳入CMB分析中。由此可知，所报道的10^{-5}量级涨落是由过度激进的前景清理引入的。
英文摘要
Within the Hot Big Bang picture, as usually interpreted in the standard LCDM framework and its hierarchical scenario for elliptical galaxy assembly, the cosmic microwave background (CMB) is associated with photon decoupling near z = 1100, and the Planck angular power spectra are taken to constrain primordial 10^{-5}-level fluctuations that seeded later structure formation. We show that, in addition to the LCDM model, two cosmological models based on Milgromian gravitation are also consistent with the Planck CMB power spectra, such that the spectra do not uniquely favor dark matter. We then argue that the published CMB spectra are not direct observables, but reconstructed quantities obtained after foreground subtraction and corrections for weak lensing, photon-electron scattering, and gravitational energy redshifts along the line of sight. Because these steps depend on the assumed growth history of structure, the resulting spectra depend on the cosmological model adopted in the data reduction. We also note that the reported correlation between the hemispherical CMB asymmetry and the excess on-sky distribution of elliptical galaxies may point to matter inhomogeneities spanning large portions of the observable universe. Motivated by observational tensions in the hierarchical assembly of elliptical galaxies, we review the consequences of elliptical-galaxy formation on a downsizing timescale, which implies a significant extragalactic foreground released at 15< z < 20. Under conservative assumptions, this foreground contributes at least 1.4 percent of the observed CMB energy density and has not been included in CMB analyses. It follows that the reported 10^{-5}-level fluctuations is introduced by overly aggressive foreground cleaning.
CommentsLatex, 24 pages, 4 figures, published in PoS (Corfu Summer Institute on Tensions in Cosmology, 2025)
Journal ref2026eppg.confE.224K
