AI 中文总结
该研究在自相互作用引力框架下修正宇宙膨胀历史，结合Union3超新星与DESI DR2 BAO数据约束参数，成功将预测光深降至与普朗克PR4测量一致的水平，缓解了JWST与CMB间的光深张力。
AI 中文摘要
近期詹姆斯·韦伯空间望远镜（JWST）的观测结果支持更早且更高效的再电离历史，导致汤姆孙散射光深大于宇宙微波背景（CMB）推断的数值。我们在自相互作用（SI）引力框架内，通过修正宇宙膨胀历史同时保留标准的再电离天体物理解释，探究是否能缓解该张力。通过对Union3 Ia型超新星与DESI DR2重子声学振荡（BAO）数据进行贝叶斯MCMC分析，约束SI引力参数，再利用所得膨胀历史预测电离历史与汤姆孙光深。研究发现，预测光深从ΛCDM模型的τ_CMB≈0.076降至τ_CMB≈0.061，与普朗克PR4测量结果在1σ范围内一致，从而大幅降低了光深张力。
英文摘要
Recent James Webb Space Telescope (JWST) observations favor an earlier and more efficient reionization history, leading to Thomson-scattering optical depths larger than those inferred from the cosmic microwave background (CMB). We investigate whether this tension can be alleviated within the framework of self-interaction (SI) gravity by modifying the cosmological expansion history while retaining the standard astrophysical description of reionization. The SI gravity parameters are constrained through a Bayesian MCMC analysis of the Union3 Type Ia supernova and DESI DR2 Baryon Acoustic Oscillations (BAO) data. The resulting expansion history is then used to predict the ionization history and Thomson optical depth. We find that the predicted optical depth decreases from $τ_{\rm{CMB}}\simeq0.076$ in $Λ$CDM to $τ_{\rm{CMB}}\simeq0.061$, consistent with the Planck PR4 measurement within $1σ$, thereby substantially reducing the optical-depth tension.
Comments26 pages, 5 Figures, 3 tables
