论文标题
重新审视了BAO+BBN - 以0.7 km/s/mpc的约束增加哈勃张力
BAO+BBN revisited -- Growing the Hubble tension with a 0.7km/s/Mpc constraint
论文作者
论文摘要
Baryonic声学振荡（BAO）数据以及来自大爆炸核合成（BBN）的光元素丰度测量的组合已被证明可将宇宙学扩展历史限制为前所未有的程度。使用来自SDSS的最新LUNA数据和DR16数据，BAO+BBN探针对Hubble参数（$ H_0 = 67.6 = 67.6 \ pm 1.0 \ pm 1.0 \ Mathrm {km/s/s/s/mpc} $）进行了严格的约束，并带有$3.7σ$3.7σ$3.7σ$3.7σ$ undension $3.7σ$张力。在更新的BAO数据中，高红移和低偏移子集在相互吻合的一致性中，并且不再存在轻度的内部张力来人为地增强约束。添加最近开发的ShapeFit分析产生$ H_0 = 68.3 \ pm 0.7 \ Mathrm {km/s/s/mpc} $（$3.8σ$张紧）。对于与其他数据集的组合，宇宙微波背景的声音范围信息具有很强的协同作用，这导致迄今为止最紧密的约束之一，$ h_0 = 68.30 \ pm 0.45 \ pm mathrm {km/s/s/s/s/mpc} $，以$4.2σ$4.2σ$ with sh0es。这种组合首选的区域与ShapeFit首选的区域完全一致。 Supernova数据的添加还产生了$4.2σ$的张力，用于万神殿的SH0ES，以及Pantheonplus的$3.5σ$张力。最后，我们表明，与哈勃张力的早期解决方案相对于BAO+BBN的约束存在一定程度的模型依赖性，并且扩展模型中约束功率的损失取决于该模型是否可以从BBN观察结果中加上额外的限制。
The combination of Baryonic Acoustic Oscillation (BAO) data together with light element abundance measurements from Big Bang Nucleosynthesis (BBN) has been shown to constrain the cosmological expansion history to an unprecedented degree. Using the newest LUNA data and DR16 data from SDSS, the BAO+BBN probe puts tight constraints on the Hubble parameter ($H_0 = 67.6 \pm 1.0 \mathrm{km/s/Mpc}$), resulting in a $3.7σ$ tension with the local distance ladder determination from SH0ES in a $Λ$CDM model. In the updated BAO data the high- and low-redshift subsets are mutually in excellent agreement, and there is no longer a mild internal tension to artificially enhance the constraints. Adding the recently-developed ShapeFit analysis yields $H_0 = 68.3 \pm 0.7 \mathrm{km/s/Mpc}$ ($3.8 σ$ tension). For combinations with additional data sets, there is a strong synergy with the sound horizon information of the cosmic microwave background, which leads to one of the tightest constraints to date, $H_0 = 68.30\pm 0.45\mathrm{km/s/Mpc}$, in $4.2σ$ tension with SH0ES. The region preferred by this combination is perfectly in agreement with that preferred by ShapeFit. The addition of supernova data also yields a $4.2σ$ tension with SH0ES for Pantheon, and a $3.5σ$ tension for PantheonPLUS. Finally, we show that there is a degree of model-dependence of the BAO+BBN constraints with respect to early-time solutions of the Hubble tension, and the loss of constraining power in extended models depends on whether the model can be additionally constrained from BBN observations.
