AI 中文总结
研究旨在确定宇宙中微子质量限制的模型依赖性，通过解构探测器对晚期物理的敏感性，采用暗能量边缘化和无晚期宇宙两条路径，得到放宽的限制，落在下一代实验室实验灵敏度范围，激发宇宙学与地面中微子测量协同。
AI 中文摘要
中微子振荡证明中微子有质量，这是标准模型之外唯一的实验室物理探测。直接运动学实验将电子中微子质量限制在\(m_{\nu_e}<0.45\)电子伏特（KATRIN，90%置信水平），意味着\(\sum m_\nu\lesssim1.3\)电子伏特。相反，\(\Lambda\)CDM中的宇宙学有很强的限制：普朗克CMB、CMB透镜化和DESI DR2 BAO得出\(\sum m_\nu<0.056\)电子伏特（95%置信水平），与反转排序下限（0.10电子伏特）有2 - 3\(\sigma\)的张力。然而，这个限制依赖于\(\Lambda\)CDM，而数据暗示暗能量在演化。为确定宇宙中微子质量限制的模型依赖性，我们解构每个探测器对晚期物理的敏感性，并采用两条稳健路径来确定\(\sum m_\nu\)的限制：（i）现有的暗能量边缘化路径，保留所有数据并对\((w_0, w_a)\)进行边缘化，结果表明它也不受灵活分箱和立方\(w(a)\)历史的影响，得出\(\sum m_\nu<0.152\)电子伏特，使用西蒙斯天文台透镜化和Spec - S5 BAO时锐化为\(\sigma(\sum m_\nu)\approx0.043\)电子伏特。（ii）一条新的无晚期宇宙路径将原始CMB通过\(A_{\rm lens}\)对声学峰值平滑进行边缘化，与重建的透镜化谱\(C_L^{\kappa\kappa}\)相结合，通过构造消除了对晚期膨胀的依赖。这得出今天\(\sum m_\nu<0.41\)电子伏特，在所有测试的暗能量模型中收紧到0.31电子伏特（西蒙斯天文台）和0.28电子伏特（宇宙方差极限）。这些放宽的限制以统计能力换取了模型独立性。有趣的是，它们落在了像项目8（\(m_{\nu_e}\sim0.1\)电子伏特）这样的下一代实验室实验的灵敏度范围内，这激发了未来宇宙学和地面中微子测量之间的重要协同作用。
英文摘要
Neutrino oscillations establish that neutrinos are massive, providing the only laboratory detection of physics beyond the Standard Model. Direct kinematic experiments bound the electron-neutrino mass to $m_{ν_e} < 0.45$ eV (KATRIN, 90% CL), implying $\sum m_ν\lesssim 1.3$ eV. Conversely, cosmology within $Λ$CDM is highly constraining: Planck CMB, CMB lensing, and DESI DR2 BAO yield $\sum m_ν< 0.056$ eV (95% CL), in 2-3$σ$ tension with the inverted-ordering floor (0.10 eV). However, this bound relies on $Λ$CDM, while data hint at an evolving dark energy. To determine the model dependence of cosmic neutrino mass bounds, we deconstruct each probe's sensitivity to late-time physics and pursue two robust routes to a $\sum m_ν$ bound: (i) The existing dark-energy-marginalized route, retaining all data and marginalizing over $(w_0, w_a)$, is shown to also be immune to flexible binned and cubic $w(a)$ histories, yielding $\sum m_ν< 0.152$ eV, sharpening to $σ(\sum m_ν) \approx 0.043$ eV with Simons Observatory lensing and Spec-S5 BAO. (ii) A new late-Universe-free route combines primary CMB, marginalizing over acoustic-peak smoothing via $A_{\rm lens}$, with the reconstructed lensing spectrum $C_L^{κκ}$, removing late-time expansion dependence by construction. This yields $\sum m_ν< 0.41$ eV today, tightening to 0.31 eV (Simons Observatory) and 0.28 eV (cosmic-variance limit) across all tested dark-energy models. These relaxed bounds trade statistical power for model independence. Interestingly, they land in the sensitivity range targeted by next-generation laboratory experiments like Project 8 ($m_{ν_e} \sim 0.1$ eV), motivating vital synergies between future cosmological and terrestrial neutrino measurements.
Comments16+7 pages, 11+5 figures, comments welcome!
