arXiv 1702.087902017-02astro-ph.CO

用Planck数据重建初始渐近de Sitter模

Reconstruction of initial Asymptotic-de Sitter mode in light of the Planck data

Hossein Moshafi, Ata Sojasi, Ebrahim Yusofi, Majid Mohsenzadeh

备注：: Changing authors

摘要：

最近公布的\emph{Planck}资料强调，暴胀的背景几何不是纯的de Sitter几何，而是从暴胀时期哈勃参数的缓慢变化来看，它可以是准de Sitter几何。这促使我们考虑一个渐近de Sitter模式函数的初始模式和曲率扰动的原始功率谱的重建。利用马尔可夫链蒙特卡罗（MCMC）方法，结合最近观测到的宇宙微波背景（CMB）数据，我们的参数化渐近初始模与纯de Sitter或Bunch-Davies模有一定的偏差。基于\emph{Planck 2015}数据发布，$ 68 \%$置信水平中标量扰动的幅度为$10^{9} A_s =2.77^{+0.32}_{-0.35}$，与Bunch-Davies模式的偏差为$\sim 0.03-0.04$。在这种参数化下，我们模型的CMB功率谱比$Λ\rm{CDM}$模型表现出更多的红倾。此外，我们发现了不同的枢轴尺度$r_{0.05}< 0.0272$和$ r_{0.002}< 0.0242$的张量标量比的上限。

英文摘要：

The recently relased \emph{Planck} data, emphasize that the background geometry of inflation is not pure de Sitter, but from the slow variation of Hubble parameter during the inflationary era, it can be quasi-de Sitter. This motivates us to consider an asymptotic de Sitter mode function for reconstruction of initial mode and primordial power spectrum of curvature perturbation. Using Markov Chain Monte Carlo (MCMC) method together with applying recent observational constraints from the Cosmic Microwave Background (CMB) data for our parametrized asymptotic initial mode shows some deviation from pure de Sitter or Bunch-Davies mode. Based on \emph{Planck 2015} data release the amplitude of scalar perturbations in $ 68 \%$ confidence level is $10^{9} A_s =2.77^{+0.32}_{-0.35}$ and deviation from Bunch-Davies mode is $\sim 0.03-0.04$. In this parametrization, the CMB power spectrum of our model shows more red-tilt in comparison with $Λ\rm{CDM}$ model. Furthermore, we found upper limit for tensor-to-scalar ratio with different pivot scales $r_{0.05}< 0.0272$ and $ r_{0.002}< 0.0242$.

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。

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