论文标题
QCDM模型中的宇宙学批量流量：（in）与$λcdm$一致性
The cosmological bulk flow in QCDM model: (In)consistency with $ΛCDM$
论文作者
论文摘要
我们通过考虑在空间平坦的宇宙学模型（FRW）空间时间和包含冷暗物质和$ Q $成分（QCDM模型）作为标量领域，并通过潜在的$ v（q）= v_ 0} exp（-λq）确定的自我交互，从而研究本地宇宙的散装流量，该模型在空间上是平坦的，（frw）空间 - 空间 - 空间和$ q $组件（QCDM模型）作为标量领域。我们使用Union 2目录的不同累积红移切片。对特殊速度的最大类似性分析证实，在低红移$ 0.015 <z <0.1 $时，批量流向$（l; b）=（302^{o} \ pm20^{o} {o} {o}; 3^{o} {o} {o} \ pm10^{o} $ v pm} = 240} = 240} = 240 = 240 = 2400 $速度。这个方向与（SSC）的方向保持一致，并与以前的数字研究一致，但是对于高红移$ 0.1 <z <0.2 $，我们得到了$ v _ {bulk} = 1000 \ pm 25kms^{ - 1} $ to $（l; b）=（l; b）=（l; b）=（l; b）=（254^{254^{+16^{+16^{O}} 6^{+7^{o}} _ { - 10^{o}}）$。这表明，对于低红移，我们的结果大致与具有最新WMAP WMAP最佳拟合宇宙学参数的$λCDM$模型一致，但是对于高红移而言，它们不同意$λcdm$，并支持以前的研究结果，例如Kashlinsky等。 Al，报告了宇宙的大量流量。我们可以得出结论，在$ QCDM $模型中，在小尺度上，暗能量的波动受到抑制，并且不会在无压物质中的扰动中输入进化方程，而在非常大的sim> sim> 100 h^{ - 1} mpc）中，它们在microwave背景的背景上留下了任何印记。
We study the bulk flow of the local universe using Type Ia supernova data by considering a class of cosmological model which is spatially flat,(FRW) space-times and contains cold dark matter and $Q$ component (QCDM models) of the fluid as a scalar field, with self interactions determined by a potential $V(Q)=V_{0}Exp(-λQ)$ evolving in Universe. We use different cumulative redshift slices of the Union 2 catalogue. A maximum-likelihood analysis of peculiar velocities confirms that at low redshift $0.015 <z<0.1$, bulk flow is moving towards the $(l; b) = (302^{o}\pm20^{o}; 3^{o}\pm10^{o})$ direction with $v _{bulk} = 240\pm 25kms^{-1} $ velocity. This direction is aligned with direction of (SSC) and agreement with a number previous studies at $(1-σ)$, however for high redshift $0.1 <z<0.2$, we get $v _{bulk} = 1000\pm 25kms^{-1} $ towards the $(l; b) = (254^{+16^{o}}_{-14^{o}}; 6^{+7^{o}}_{-10^{o}})$. This indicates that for low redshift our results are approximately consistent with the $ΛCDM$ model with the latest WMAP best fit cosmological parameters however for high redshift they are in disagreement of $ΛCDM$ and support the results of previous studies such as Kashlinsky et. al, which report the large bulk flow for the Universe. We can conclude that, in $QCDM$ model, at small scales, fluctuations of the dark energy are damped and do not enter in the evolution equation for the perturbations in the pressureless matter, while at very large scales $(\sim > 100 h^{-1}Mpc)$, they leaving an imprint on the microwave background anisotropy.
