关于暗能量空洞和超密度的量级
On the Magnitude of Dark Energy Voids and Overdensities
摘要：
我们研究了暗能量在物质超密度和空洞中的聚集。特别是，我们推导出一个解析表达式的暗能量密度扰动，这是有效的线性，准线性和完全非线性制度的结构形成。我们还研究了通过ISW效应探测这种暗能量聚集的可能性。在非耦合的精粹模型的情况下，如果场的质量是今天的哈勃尺度或更小，那么与物质密度对比度相比，暗能量波动总是很小的。即使当物质扰动进入非线性区域时，暗能量扰动仍然保持线性。我们发现，维里化集群和空洞对应于局部超密度在暗能量，与$δ_ϕ/(1+w) \sim \Oo(10^{-5})$的空洞，$δ_ϕ/(1+w) \sim \Oo(10^{-4})$的超级空洞和$δ_ϕ/(1+w) \sim \Oo(10^{-5})$的一个典型的维里化集群。如果在可见宇宙中存在半径为$100-300 {\rm Mpc}$的空洞，那么$δ_ϕ$可能和$10^{-3}(1+w)$一样大。物质和超星系团的线性超密度通常对应于暗能量中的局部空洞;对于一个典型的超星系团：$δ_ϕ/(1+w) \sim \Oo(-10^{-5})$。在这项工作中采取的方法可以直接扩展到研究更一般的暗能量模型的聚类。
英文摘要：
We investigate the clustering of dark energy within matter overdensities and voids. In particular, we derive an analytical expression for the dark energy density perturbations, which is valid both in the linear, quasi-linear and fully non-linear regime of structure formation. We also investigate the possibility of detecting such dark energy clustering through the ISW effect. In the case of uncoupled quintessence models, if the mass of the field is of order the Hubble scale today or smaller, dark energy fluctuations are always small compared to the matter density contrast. Even when the matter perturbations enter the non-linear regime, the dark energy perturbations remain linear. We find that virialised clusters and voids correspond to local overdensities in dark energy, with $δ_ϕ/(1+w) \sim \Oo(10^{-5})$ for voids, $δ_ϕ/(1+w) \sim \Oo(10^{-4})$ for super-voids and $δ_ϕ/(1+w) \sim \Oo(10^{-5})$ for a typical virialised cluster. If voids with radii of $100-300 {\rm Mpc}$ exist within the visible Universe then $δ_ϕ$ may be as large as $10^{-3}(1+w)$. Linear overdensities of matter and super-clusters generally correspond to local voids in dark energy; for a typical super-cluster: $δ_ϕ/(1+w) \sim \Oo(-10^{-5})$. The approach taken in this work could be straightforwardly extended to study the clustering of more general dark energy models.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
