AI 中文总结
该研究结合多类观测数据，分析空间曲率与动力学暗能量对谱指数的影响，发现扩展宇宙学模型可缓解观测数据与三类暴胀模型的张力，相关模型对未来巡天研究有重要意义。
AI 中文摘要
我们结合宇宙微波背景数据集（普朗克Planck、南极望远镜SPT、阿塔卡马宇宙学望远镜ACT）以及暗能量光谱仪DESI的光谱星系样本（包含重子声学振荡BAO和全形成团测量），研究空间曲率（Ωₖ）与动力学暗能量（以w₀和wₐ参数化）对谱指数nₛ的影响。结果显示，小的负曲率Ωₖ≈3×10⁻³会降低nₛ值，使其更接近Starobinsky模型、希格斯模型及最简α吸引子暴胀模型的预测：使用Planck与DESI数据时nₛ=0.9667±0.0041，加入ACT和SPT后nₛ=0.9692±0.0035。允许暗能量随时间演化也会降低谱指数，联合数据集下nₛ=0.9716±0.0032，结合小负曲率时nₛ=0.9694±0.0035。研究表明，当前观测数据与Starobinsky模型、希格斯模型及最简α吸引子模型的张力仅存在于ΛCDM模型中，在扩展宇宙学模型中可得到缓解。我们讨论了这些发现对开放宇宙及/或含动力学暗能量的暴胀模型的意义，包括量子隧穿和非标准拓扑场景，还简要描述了一类特殊的α吸引子模型（可使nₛ任意大）及α吸引子 quintessence模型，这类模型对未来DESI、DESI-II、SPHEREx、Euclid、鲁宾望远镜Rubin、罗曼望远镜Roman的数据研究具有重要意义。
英文摘要
We study the impact of spatial curvature ($Ω_k$) and dynamical dark energy (parametrized by $w_0$ and $w_a$) on the spectral index $n_s$ using a combination of cosmic microwave background datasets (Planck, SPT, and ACT), and spectroscopic galaxy samples from DESI, including both BAO and full-shape clustering measurements. We show that a small negative curvature, $Ω_k\simeq 3\times 10^{-3}$, lowers the value of $n_s$, bringing it closer to predictions of the Starobinsky, Higgs, and simplest $α$-attractor inflationary models. In particular, we find $n_s= 0.9667\pm0.0041$ (using Planck and DESI data) or $n_s= 0.9692\pm0.0035$ (adding ACT and SPT). Allowing for time-evolving dark energy also reduces the spectral index, leading to $n_s=0.9716\pm0.0032$ (from the combined dataset), or $n_s=0.9694\pm0.0035$ in combination with a small negative curvature. Our results demonstrate that the tension between current observational data and the Starobinsky, Higgs, and simplest $α$-attractor models holds only for $Λ$CDM, and can be mitigated in extended cosmological models. We discuss implications of these findings for inflationary models in an open universe and/or with dynamical dark energy, including scenarios with quantum tunneling and non-standard topology. Furthermore, we briefly describe a special class of $α$-attractor models, where one can make $n_s$ arbitrarily large, and we describe the $α$-attractor quintessence model. Such models may be of particular relevance when future data from DESI, as well as DESI-II, SPHEREx, Euclid, Rubin, and Roman, becomes available.
Comments29 pages, 5 figures, 2 tables;
