Cluster probes of dark energy clustering
Cluster probes of dark energy clustering
复制标题
暗能量聚类的簇探针
DOI：
10.1103/physrevd.88.043526
复制
发表时间：
2013
影响因子：
5
通讯作者：
J. Weller
中科院分区：
文献类型：
--
作者：
S. Appleby;E. Linder;J. Weller
奇怪的是，星系团的丰度对典型的早期暗能量不敏感。早期的暗能量的声速等于光速，不能从一个具有等效膨胀历史的精粹模型中区分出来，因为z<2，但早期的暗能量密度可以忽略不计，尽管早期的增长率不同。然而，早期的冷暗能量，其声速比光速小得多，可以提供可检测的签名。结合星团丰度和宇宙微波背景功率谱可以确定早期暗能量分数为0.3%，并在99%的置信度下区分真实声速为0.1和1。我们从欧几里得星系团调查，以及暗能量调查项目的限制，使用当前和预计的普朗克CMB数据，并评估集群质量系统学的影响。我们还量化了暗能量扰动的重要性，以及声速在$w=-1$穿越过程中的作用。
Cluster abundances are oddly insensitive to canonical early dark energy. Early dark energy with sound speed equal to the speed of light cannot be distinguished from a quintessence model with the equivalent expansion history for $z<2$ but negligible early dark energy density, despite the different early growth rate. However, cold early dark energy, with a sound speed much smaller than the speed of light, can give a detectable signature. Combining cluster abundances with cosmic microwave background power spectra can determine the early dark energy fraction to 0.3 % and distinguish a true sound speed of 0.1 from 1 at 99 % confidence. We project constraints on early dark energy from the Euclid cluster survey, as well as the Dark Energy Survey, using both current and projected Planck CMB data, and assess the impact of cluster mass systematics. We also quantify the importance of dark energy perturbations, and the role of sound speed during a crossing of $w=-1$.