论文标题
在宇宙学尺度上首次直接测量重力潜在衰减速率并改善了深色能量约束
The first direct measurement of gravitational potential decay rate at cosmological scales and improved dark energy constraint
论文作者
论文摘要
集成的Sachs-Wolfe（ISW）效应探测了大规模重力潜力的衰减率（$ dr $），因此对暗能量（DE）提供了独特的约束。但是，其约束功率因ISW测量而降低，ISW测量依赖于与大规模结构（LSS）的交叉相关性，并且在银河系偏差和物质聚类中遭受了不确定性。结合Lensing-LSS互相关的结合，$ DR $可以在没有银河系偏见和物质聚类中的不确定性的方式隔离。我们将此建议应用于DESI成像调查的DR8 Galaxy目录和Planck Cosmic微波背景（CMB）地图的组合。我们实现了第一个$ DR $测量值，总重要性为$3.2σ$。我们验证了三个红移垃圾箱（$ [0.2,0.4）$，$ [0.4，0.6）$，$ [0.6,0.8] $）的测量结果，其中有两个LSS示踪剂（“低密度点”和常规的银河位置）。尽管S/N相对较低，但$ DR $的添加显着改善了暗能量的限制，仅SDSS Baryon声学振荡（BAO）数据或单独使用Pantheon Supernovae（SN）汇编。对于Flat $ w $ CDM宇宙学，$ω_m$的精度的提高比BAO比1.8倍，而SN的倍数为1.5。对于国家$ W $的DE等式，BAO的改进因子为1.3，而SN的改进因子为1.4。这些改进证明了$ DR $是一种有用的宇宙学探测，因此我们主张其在未来的宇宙学分析中的用法。
The integrated Sachs-Wolfe (ISW) effect probes the decay rate ($DR$) of large scale gravitational potential and therefore provides unique constraint on dark energy (DE). However its constraining power is degraded by the ISW measurement, which relies on cross-correlating with the large scale structure (LSS) and suffers from uncertainties in galaxy bias and matter clustering. In combination with lensing-LSS cross-correlation, $DR$ can be isolated in a way free of uncertainties in galaxy bias and matter clustering. We applied this proposal to the combination of the DR8 galaxy catalogue of DESI imaging surveys and Planck cosmic microwave background (CMB) maps. We achieved the first $DR$ measurement, with a total significance of $3.2σ$. We verified the measurements at three redshift bins ($[0.2,0.4)$, $[0.4, 0.6)$, $[0.6,0.8]$), with two LSS tracers (the "low-density points" and the conventional galaxy positions). Despite its relatively low S/N, the addition of $DR$ significantly improves dark energy constraints, over SDSS baryon acoustic oscillation (BAO) data alone or Pantheon supernovae (SN) compilation alone. For flat $w$CDM cosmology, the improvement in the precision of $Ω_m$ is a factor of 1.8 over BAO and 1.5 over SN. For the DE equation of state $w$, the improvement factor is 1.3 over BAO and 1.4 over SN. These improvements demonstrate $DR$ as a useful cosmological probe, and therefore we advocate its usage in future cosmological analysis.
