A Better Reconciliation of Hubble Tension in the Dark Energy Scalar Field  

作　　者：Le Fu Li Chen Maoyou Yang Junmei Wang Ming-Jian Zhang 

机构地区：[1]School of Information and Automation Engineering,Qilu University of Technology(Shandong Academy of Sciences),Jinan 250353,China [2]International School for Optoelectronic Engineering,Qilu University of Technology(Shandong Academy of Sciences),Jinan 250353,China

出　　处：《Research in Astronomy and Astrophysics》2023年第3期37-45,共9页天文和天体物理学研究（英文版）

基　　金：Ming-Jian Zhang is supported by the Natural Science Foundation of Shandong Province(Grant No.ZR2021MA075);Li Chen is supported by the Natural Science Foundation of Shandong Province(Grant No.ZR2019MA033)。

摘　　要：Hubble tension between the local measurement and global observation has been a key problem in cosmology.In this paper,we consider the quintessence scalar field,phantom field and quintom field as the dark energy to reconcile this problem.Different from most previous work,we start from the dimensionless equation of state(w)of dark energy,not a parameterization of potential.The combined analysis shows that observational data sets favor Hubble constant H0=71.3-0.917+0.854 km s^(-1)Mpc^(-1),which can reconcile Hubble tension within 1.20σ.We also perform a Bayes factor analysis using the MCEvidence code,and confirm that the phantom scalar field is still the most effective.To investigate the reason of Hubble tension,we analyze the density parameter.The comparison shows that the scalar fields provide a slightly largerΩbh2 and smallerΩch2 than the standardΛCDM model.We finally analyze a possible reason of Hubble tension from the kinematic acceleration?.We find an interesting physical phenomenon.The acceleration a in these scalar fields are similar as theΛCDM model at about redshift z>0.5.However,they increase and deviate from each other at low redshift,especially in the near future.Only the?in phantom scalar field will decrease in the future.

关 键 词：PARAMETER potential OBSERVATIONAL 

分 类 号：P145.9[天文地球—天体物理] P111[天文地球—天文学]