arXiv 2204.070992022-04astro-ph.CO

利用哈勃测量直接估计$\Lambda$CDM宇宙的密度参数和哈勃常数

On Direct Estimation of Density Parameters and Hubble Constant for $Λ$CDM Universe using Hubble Measurements

Srikanta Pal, Rajib Saha

备注：: 21 pages, 6 figures, 5 tables
发表信息：: Physica Scripta 99 (2024) 085025
DOI：: 10.1088/1402-4896/ad5f5b

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AI总结：

本文提出一种利用哈勃参数测量直接估计非平坦$\Lambda$CDM宇宙密度参数和哈勃常数的新方法，无需依赖其他参数，结果与Planck数据一致。

摘要：

一组宇宙学密度参数（$\Omega_{0m}h_{0}^{2}$、$\Omega_{0k}h_{0}^{2}$、$\Omega_{0\Lambda}h_{0}^{2}$）和哈勃常数（$\hat{h}_{0}$）对于从多个角度理解宇宙的基本性质非常有用。在本文中，我们提出了一种新方法来估计Friedmann-Robertson-Walker（FRW）背景下的$\Lambda$冷暗物质（$\Lambda$CDM）宇宙的这些参数。我们将Sahni等人（2008）首次提出的两点统计量推广到三点情形，并利用目前可用的哈勃参数（$H(z)$）测量值（红移范围$0.07 \leq z \leq 2.36$，通过微分年龄（DA）和重子声学振荡（BAO）技术测得）来估计这些参数。所有参数均在非平坦宇宙的一般情形下进行估计。使用DA和BAO数据，我们得到$\Omega_{0m}h_{0}^{2}=0.1485 \pm 0.0065$、$\Omega_{0k}h_{0}^{2}=-0.0137 \pm 0.017$、$\Omega_{0\Lambda}h_{0}^{2}=0.3126 \pm 0.0145$以及$\hat{h}_{0}=0.6689 \pm 0.0021$。这些结果与Planck结果令人满意地一致。我们方法的一个重要优势是，估计任何独立宇宙学参数的值时，无需使用其余参数的值。每个参数仅根据不同红移处的哈勃参数测量值获得，无需使用其他参数的值。这种方法预计在参数估计过程中较少受到宇宙学参数之间简并问题的不利影响。此外，我们的方法不需要假设空间平坦性。

英文摘要：

The set of cosmological density parameters ($Ω_{0m}h_{0}^{2}$, $Ω_{0k}h_{0}^{2}$, $Ω_{0Λ}h_{0}^{2}$) and Hubble constant ($\hat{h}_{0}$) are useful for fundamental understanding of the universe from many perspectives. In this article, we propose a new procedure to estimate these parameters for $Λ$ cold dark matter ($Λ$CDM) universe in the Friedmann-Robertson-Walker (FRW) background. We generalize the two-point statistics first proposed by Sahni et al. (2008) to the three point case and estimate the parameters using currently available Hubble parameter ($H(z)$) values in the redshift range $0.07 \leq z \leq 2.36$ measured by differential age (DA) and baryon acoustic oscillation (BAO) techniques. All the parameters are estimated assuming the general case of non-flat universe. Using both DA and BAO data we obtain $Ω_{0m}h_{0}^{2}=0.1485 \pm 0.0065$, $Ω_{0k}h_{0}^{2}=-0.0137 \pm 0.017$, $Ω_{0Λ}h_{0}^{2}=0.3126 \pm 0.0145$ and $\hat{h}_{0}=0.6689 \pm 0.0021$. These results are in satisfactory agreement with the Planck results. An important advantage of our method is that to estimate the value of any one of the independent cosmological parameters one does not need to use the values for the rest of them. Each parameter is obtained solely from the measured values of Hubble parameters at different redshifts without any need to use values of other parameters. Such a method is expected to be less susceptible to the undesired effects of degeneracy issues between cosmological parameters during their estimations. Moreover, there is no requirement of assuming spatial flatness in our method.

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