利用普朗克 PR4、DESI 重子声学振荡和超新星更新扩展参数空间的宇宙学约束:动态暗能量、中微子质量、透镜反常和哈勃张力

Shouvik Roy Choudhury and Teppei Okumura
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引用次数: 0

摘要

我们提出了 12 参数模型中宇宙学参数的最新约束,通过包括动态暗能量(DE;w0,wa)、中微子质量总和(∑mν)、非光子辐射物种的有效数量(Neff)、透镜振幅缩放(Alens)和标量光谱指数(αs)的运行,扩展了标准六参数ΛCDM。对于宇宙波背景(CMB)数据,我们使用了普朗克公开发布(PR)4(2020)HiLLiPoP和LoLLiPoP似然、普朗克PR4+阿塔卡马宇宙学望远镜(ACT)DR6透镜和普朗克2018低ℓ TT似然,以及DESI DR1重子声振荡(BAO)和Pantheon+和DESY5未经校准的Ia型超新星(SNe)似然。主要发现如下(i) 与DESI结果相反,CMB+BAO+Pantheon+数据在2σ以内包含了一个宇宙常数,而CMB+BAO+DESY5则在超过2σ时将其排除在外,这表明DE的动力学性质尚不稳定。DESY5 样本中潜在的系统性可能会导致这种排除。(ii) 一些数据组合显示对非零∑mν的探测达到了1σ+,这表明未来有可能进行探测。我们还提供了 ∑mν ≲ 0.3 eV 的稳健上限(95% 置信限)。(iii) 使用 CMB+BAO+SNe 时,Alens = 1 在 2σ 时被包含在内(尽管不是在 1σ),这表明在普朗克 PR4 可能性的这一扩展宇宙学中没有明显的透镜异常。(iv) 哈勃张力持续存在于 3.2 至 3.9σ,表明这些简单的扩展并不能解决它。(v) 暗能量巡天第三年弱透镜的 S8 张力减小到 1.4σ,这可能是由于附加参数和普朗克 PR4 可能性造成的。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Updated Cosmological Constraints in Extended Parameter Space with Planck PR4, DESI Baryon Acoustic Oscillations, and Supernovae: Dynamical Dark Energy, Neutrino Masses, Lensing Anomaly, and the Hubble Tension
We present updated constraints on cosmological parameters in a 12-parameter model, extending the standard six-parameter ΛCDM by including dynamical dark energy (DE; w0, wa), the sum of neutrino masses (∑mν), the effective number of non-photon radiation species (Neff), the lensing amplitude scaling (Alens), and the running of the scalar spectral index (αs). For cosmic wave background (CMB) data, we use the Planck Public Release (PR) 4 (2020) HiLLiPoP and LoLLiPoP likelihoods, Planck PR4+Atacama Cosmology Telescope (ACT) DR6 lensing, and Planck 2018 low-ℓ TT likelihoods, along with DESI DR1 baryon acoustic oscillations (BAO) and Pantheon+ and DESY5 uncalibrated Type Ia supernovae (SNe) likelihoods. Key findings are the following: (i) Contrary to DESI results, CMB+BAO+Pantheon+ data include a cosmological constant within 2σ, while CMB+BAO+DESY5 excludes it at over 2σ, indicating the dynamical nature of DE is not yet robust. Potential systematics in the DESY5 sample may drive this exclusion. (ii) Some data combinations show a 1σ+ detection of nonzero ∑mν, indicating possible future detection. We also provide a robust upper bound of ∑mν ≲ 0.3 eV (95% confidence limit (CL)). (iii) With CMB+BAO+SNe, Alens = 1 is included at 2σ (albeit not at 1σ), indicating no significant lensing anomaly in this extended cosmology with Planck PR4 likelihoods. (iv) The Hubble tension persists at 3.2 to 3.9σ, suggesting these simple extensions do not resolve it. (v) The S8 tension with Dark Energy Survey Year 3 weak lensing is reduced to 1.4σ, likely due to additional parameters and the Planck PR4 likelihoods.
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