论文标题
将深色能量烙印在引力场的宇宙学观察物上
Clustering dark energy imprints on cosmological observables of the gravitational field
论文作者
论文摘要
我们在聚集暗能量的背景下研究固定观察者的过去光锥上的宇宙学可观察力。我们专注于直接探测重力场的可观察物，即综合的sachs-wolfe和非线性rees-sciama效应（ISW-RS），弱重力透镜，重力红移和夏皮罗时间延迟。借助我们的专用$ n $体制代码“ $ k $ - 进化”，跟踪了暗物质粒子和深色能源场的耦合演变，我们能够研究低速$ C_S $的制度，其中暗能量扰动可能会变得很大。使用射线跟踪，我们为每种效果生成二维天空图，并计算它们的角功率谱。事实证明，ISW-RS信号是限制以$ W-C_S^2 $来限制聚类的暗能特性的最有前途的探测器，因为$ \ textit {Linearear} $ clustering of Dark Energy将角度频谱通过$ \ sim 30 \％\％$ \％$在低$ \ ell $ flust $ \ ell $ for Diffe of Sound的速度时将角功率谱从$ \％\％\％\％变化。弱重力镜头，夏皮罗时间延迟和重力红移是群集黑能的敏感探针，仅显示几个百分比的变化。在所有功率谱中，深色能量$ \ textit {non-linearities} $在低$ \ ell $时都可以忽略不计，但分别达到$ 2 \％$和$ 3 \％$，在收敛和ISW-rs Angular Power Spectra中，在redshift $ \ sim 0.85 $ 0.85 $ 0.85。未来的宇宙学调查达到精度测量百分比将允许探测深色能量的聚类至高度的信心。
We study cosmological observables on the past light cone of a fixed observer in the context of clustering dark energy. We focus on observables that probe the gravitational field directly, namely the integrated Sachs-Wolfe and non-linear Rees-Sciama effect (ISW-RS), weak gravitational lensing, gravitational redshift and Shapiro time delay. With our purpose-built $N$-body code "$k$-evolution" that tracks the coupled evolution of dark matter particles and the dark energy field, we are able to study the regime of low speed of sound $c_s$ where dark energy perturbations can become quite large. Using ray tracing we produce two-dimensional sky maps for each effect and we compute their angular power spectra. It turns out that the ISW-RS signal is the most promising probe to constrain clustering dark energy properties coded in $w-c_s^2$, as the $\textit{linear}$ clustering of dark energy would change the angular power spectrum by $\sim 30\%$ at low $\ell$ when comparing two different speeds of sound for dark energy. Weak gravitational lensing, Shapiro time-delay and gravitational redshift are less sensitive probes of clustering dark energy, showing variations of a few percent only. The effect of dark energy $\textit{non-linearities}$ in all the power spectra is negligible at low $\ell$, but reaches about $2\%$ and $3\%$, respectively, in the convergence and ISW-RS angular power spectra at multipoles of a few hundred when observed at redshift $\sim 0.85$. Future cosmological surveys achieving percent precision measurements will allow to probe the clustering of dark energy to a high degree of confidence.
