In this work, we investigate the recently introduced phenomenological emergent dark energy (PEDE) model and the anisotropic extension of PEDE ($\mathcal{A}$PEDE) via Bianchi type-I spacetime metric with the latest observational data involving both low and high redshift datasets as, Hubble, Cosmic Microwave Background (CMB), Baryon Acoustic Oscillations (BAO) and Pantheon. We perform Bayesian inference analysis to carry out a detailed comparison of these models with the standard $\Lambda$CDM and anisotropic $\Lambda$CDM ($\mathcal{A}\Lambda$CDM) models. The 68% confidence limit (CL) constraints on Hubble constant with joint data combination for both PEDE and $\mathcal{A}$PEDE models yield $H_0=70.8\pm 0.5{\mathrm{km s}}^{-1}{\mathrm{Mpc}}^{-1}$, consistent with the local value $H_0=69.8\pm 0.8{\mathrm{km s}}^{-1}{\mathrm{Mpc}}^{-1}$ based on a calibration of the Tip of the Red Giant Branch applied to supernovae Type Ia. In addition, this value provides $\sim 2.1\sigma$ tension in comparison with the local measurement value $74.03\pm 1.42{\mathrm{km s}}^{-1}{\mathrm{Mpc}}^{-1}$ from Hubble Space Telescope observations of Cepheids in the Large Magellanic Cloud. The phantom like behaviour of dark energy in PEDE and $\mathcal{A}$PEDE models lead to an early redshift transition in comparison with $\Lambda$CDM and $\mathcal{A}\Lambda$CDM models. Further, we observe that the upper bound on the expansion anisotropy parameter ${\Omega }_{\sigma 0}$ for $\mathcal{A}$PEDE at 95% CL is approximately of the order $10^{-18}$ with all data combinations, unable to make any relevant change in the CMB quadrupole problem. Moreover, we find that the expansion anisotropy for $\mathcal{A}$PEDE ($\mathcal{A}\Lambda$CDM) model does not alter the conclusions for PEDE ($\Lambda$CDM) model. The statistical results for both PEDE and $\mathcal{A}$PEDE models in comparison with the base $\Lambda$CDM show a good fit with the data combination of Hubble+CMB, while the addition of BAO or Pantheon with other data combinations lead to a very strong evidence against the PEDE models.

在这项工作中，我们研究了最近引入的现象学新兴暗能量（PEDE）模型和PEDE的各向异性扩展（$\mathcal{一种}$PEDE）通过Bianchi I型时空度量标准，并具有最新的观测数据，涉及低和高红移数据集，如哈勃，宇宙微波背景（CMB），重子声振荡（BAO）和万神殿。我们执行贝叶斯推理分析，以将这些模型与标准进行详细比较$\Lambda$CDM和各向异性 $\Lambda$CDM（$\mathcal{一种}\Lambda$CDM）模型。PEDE和PEDE的联合数据组合对Hubble常数的68％置信限（CL）约束$\mathcal{一种}$PEDE模型收益 $H_0=70。8\pm 0。5{\mathrm{公里}}^{-\mathrm{1个}}{\mathrm{Mpc}}^{-\mathrm{1个}}$，与当地价值一致 $H_0=69。8\pm 0。8{\mathrm{公里}}^{-\mathrm{1个}}{\mathrm{Mpc}}^{-\mathrm{1个}}$基于对适用于Ia型超新星的红色巨人分支尖端的校准。此外，此值还提供$〜2。\mathrm{1个}\sigma$ 张力与局部测量值的比较 $74。03\pm \mathrm{1个}。42{\mathrm{公里}}^{-\mathrm{1个}}{\mathrm{Mpc}}^{-\mathrm{1个}}$来自哈勃太空望远镜对麦哲伦星云中造父变星的观测。PEDE和中的暗能量的幻像状行为$\mathcal{一种}$与之相比，PEDE模型导致了早期的红移过渡 $\Lambda$CDM和 $\mathcal{一种}\Lambda$CDM模型。此外，我们观察到膨胀各向异性参数的上限${\Omega }_{\sigma 0}$ 对于 $\mathcal{一种}$PEDE在95％CL左右的量级 $\mathrm{1个}{0}^{-\mathrm{18岁}}$所有数据组合都无法在CMB四极杆问题上进行任何相关更改。此外，我们发现$\mathcal{一种}$PEDE（$\mathcal{一种}\Lambda$CDM）模型不会改变PEDE（$\Lambda$CDM）模型。PEDE和$\mathcal{一种}$PEDE模型与基础比较 $\Lambda$CDM与Hubble + CMB的数据组合非常吻合，而BAO或Pantheon与其他数据组合的结合则为反对PEDE模型提供了非常有力的证据。