论文标题
哈勃张力中的空隙？哈勃气泡的线路末端
A void in the Hubble tension? The end of the line for the Hubble bubble
论文作者
论文摘要
宇宙可能具有超出标准范式的大规模不均匀性，这意味着统计均匀性和各向同性只能在比通常假定的$ \ sim $ 100 MPC的情况下达到。这意味着我们不一定是典型的观察者，哥白尼原理只能在超级超级尺度上恢复。 Here, we do not assume the validity of the Copernican principle and let Cosmic Microwave Background, Baryon Acoustic Oscillations, type Ia supernovae, local $H_0$, cosmic chronometers, Compton y-distortion and kinetic Sunyaev-Zeldovich observations constrain the geometrical degrees of freedom of the local structure, which we parametrize via the $Λ$LTB model -- basically a FLRW度量的非线性径向扰动。为了量化非欧洲结构是否可以解释哈勃张力，我们要仔细注意计算不均匀宇宙中的哈勃常数，并且我们通过贝叶斯因素和Akaike信息标准采用模型选择。我们的结果表明，尽管$λ$ LTB型号可以成功解释$ H_0 $张力，但仅当一个人仅考虑用于适合哈勃常数的红移范围内的超新星时，它才受到$λ$ CDM模型的青睐，但$ 0.023 <z <z <z <0.15 $。如果人们考虑了所有超新星样本，则无法解决$ H_0 $张力，并且对$λ$ LTB型号的支持消失了。与其他数据集结合使用，对哈勃张力的解决方案几乎无济于事。最后，我们重建了当地的时空。我们发现，具有$δ_l\ $Δ_l\左右的浅空效率和$ r^{\ mathrm {out}} _ l \ 300 $ MPC最好拟合数据，这与标准模型预期相对于95 \％可信区域的边界很有趣。
The Universe may feature large-scale inhomogeneities beyond the standard paradigm, implying that statistical homogeneity and isotropy may be reached only on much larger scales than the usually assumed $\sim$100 Mpc. This means that we are not necessarily typical observers and that the Copernican principle could be recovered only on super-Hubble scales. Here, we do not assume the validity of the Copernican principle and let Cosmic Microwave Background, Baryon Acoustic Oscillations, type Ia supernovae, local $H_0$, cosmic chronometers, Compton y-distortion and kinetic Sunyaev-Zeldovich observations constrain the geometrical degrees of freedom of the local structure, which we parametrize via the $Λ$LTB model -- basically a non-linear radial perturbation of a FLRW metric. In order to quantify if a non-Copernican structure could explain away the Hubble tension, we pay careful attention to computing the Hubble constant in an inhomogeneous universe, and we adopt model selection via both the Bayes factor and the Akaike information criterion. Our results show that, while the $Λ$LTB model can successfully explain away the $H_0$ tension, it is favored with respect to the $Λ$CDM model only if one solely considers supernovae in the redshift range that is used to fit the Hubble constant, that is, $0.023<z<0.15$. If one considers all the supernova sample, then the $H_0$ tension is not solved and the support for the $Λ$LTB model vanishes. Combined with other data sets, this solution to the Hubble tension barely helps. Finally, we have reconstructed our local spacetime. We have found that data are best fit by a shallow void with $δ_L \approx -0.04$ and $r^{\mathrm{out}}_L \approx 300$ Mpc, which, interestingly, lies on the border of the 95\% credible region relative to the standard model expectation.
