Measuring dark energy clustering with CMB-galaxy correlations
Measuring dark energy clustering with CMB-galaxy correlations
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DOI：
10.1103/physrevd.70.123002
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发表时间：
2004-08
影响因子：
5
通讯作者：
Wayne Hu;R. Scranton
中科院分区：
文献类型：
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作者：
Wayne Hu;R. Scranton
通过与星系的相关性测量的宇宙微波背景中的综合萨克斯-沃尔夫效应提供了一个独特的机会，通过其大尺度聚类特性来研究暗能量的动力学。最终，一个深度为z{approx}2的全天星系调查可以对相关性进行{approx}10{sigma}或{approx}10%的测量，并限制由于Gpc尺度上的暗能量聚集而导致的引力势或总密度波动的{approx}3%的变化。一个典型的单标量场或quintessence模型预测，这些集群效应将出现在视界尺度上，其强度反映了暗能量密度的演变。在恒定状态方程方面，这将允许测试垂直条1+w垂直条>或近似的模型的精华预测。0.05.
The integrated Sachs-Wolfe effect in the cosmic microwave background as measured through its correlation with galaxies provides a unique opportunity to study the dynamics of the dark energy through its large scale clustering properties. Ultimately, a deep all-sky galaxy survey out to z{approx}2 can make a {approx}10{sigma} or {approx}10% measurement of the correlation and limit {approx}3% changes in the gravitational potential or total density fluctuation due to dark energy clustering on the Gpc scale. A canonical single scalar field or quintessence model predicts that these clustering effects will appear on the horizon scale with a strength that reflects the evolution of the dark energy density. In terms of a constant equation of state, this would allow tests of the quintessence prediction for models where vertical bar 1+w vertical bar > or approx. 0.05.