论文标题
直接估计密度参数和哈勃常数$λ$ CDM宇宙，使用哈勃测量
On Direct Estimation of Density Parameters and Hubble Constant for $Λ$CDM Universe using Hubble Measurements
论文作者
论文摘要
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从许多角度来看宇宙。在本文中，我们提出了一个新的程序，以估算$λ$冷暗物质（$λ$ cdm）宇宙的这些参数在Friedmann-Robertson-Walker（FRW）背景中。我们概括了Sahni等人首先提出的两点统计。 （2008）到三个点案例，并使用当前可用的哈勃参数（$ h（z）$）值在红移范围内估算参数$ 0.07 \ leq z \ leq z \ leq 2.36 $，通过差异年龄（DA）和Baryon Acousttic Osciltic Oscillation（bao）技术测量。所有参数均被估计，假设非平板宇宙的一般情况。使用DA和BAO数据，我们获得了$ω_{0M} H_ {0}^{2} = 0.1485 \ pm 0.0065 $，$ω__{0K} h_ {0}^0}^{2} = -0.0137 \ pm 0.0145 $和$ \ hat {h} _ {0} = 0.6689 \ pm 0.0021 $。这些结果与普朗克的结果达成了令人满意的一致性。我们方法的一个重要优点是，要估计一个独立的宇宙学参数的价值，就不需要为其其余的值使用这些值。每个参数仅从不同红移的哈勃参数的测量值中获得，而无需使用其他参数的值。预计这种方法在估计期间宇宙学参数之间的堕落问题不良影响不太容易受到影响。此外，不需要在我们的方法中假设空间平坦。
The set of cosmological density parameters ($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.
