哈勃参量观测数据及其他数据对相互作用暗能量的观测限制

Constraints on the interacting dark energy with Hubble parameter data and other observational data

主要基于哈勃参量观测数据(OHD)、普朗克卫星的微波背景辐射数据(CMB)、重子声学振荡数据(BAO)和Ia型超新星数据(SNe)来限制宇宙学相互作用暗能量模型.利用马尔可夫链蒙特卡洛(MCMC)算法和Cosmo MC程序,用c2的方法实现模型中参数的数值拟合.OHD+SNe+CMB+BAO数据组合得到各参数的最佳拟合值及2s误差范围分别为:物质密度参数ΩW=m0.2919+0.0075-0.0075(1σ)+0.0151-0.0144(2σ),暗能量状态方程参数wX=-1.0374+0.0453-0.0452(1σ)+0.0898-0.0886(2σ)哈勃常数H0=69.6479+0.85809-0.8563(1σ)+1.6919-1.6768(2σ)相互作用因子=3.0976+0.1600-0.1609(1σ)+0.3153-0.3189(2σ)wx,的最佳拟合值满足+3<0wX即暗能量趋于转化为暗物质,表明宇宙学巧合性问题被轻微缓解.为了研究OHD对相互作用参数的限制效果,本文采用OHD,SNe和CMB+BAO数据组合对该模型进行了限制对比,得到结论如下:(1)当联合SNe,CMB+BAO,OHD能更紧密地限制相互作用暗能量模型,并且OHD具有缓解巧合性问题的潜力;(2)对于LCDM模型中+3wx表示暗物质和暗能量无相互作用的情形均包括在OHD+CMB+BAO,SNe+CMB+BAO,和OHD+SNe+CMB+BAO三组数据限制结果的1s范围.

We constrain an interacting dark energy model with the Hubble parameter data（OHD）,as well as the cosmic microwave background（CMB） observations from the Planck first data release,the baryonic acoustic oscillation（BAO） observations and the type Ia supernovae（SNe） data. The model parameters are determined by applying the maximum likelihood method of c2 fitting by using the Markov Chain Monte Carlo（MCMC） method. The best-fit values of the model parameters with OHD＋ SNe＋CMB＋BAO are ΩW=m0.2919＋0.0075-0.0075（1σ）＋0.0151-0.0144（2σ） wX=-1.0374＋0.0453-0.0452（1σ）＋0.0898-0.0886（2σ）=3.0976＋0.1600-0.1609（1σ）＋0.3153-0.3189（2σ） H0=69.6479＋0.85809-0.8563（1σ）＋1.6919-1.6768（2σ）The energy is transferred from dark energy to dark matter. The coincidence problem is slightly alleviated in 1σ range. For comparison,we constrain this model with OHD＋BAO＋CMB and SNe＋CMB＋BAO. The results are as follows：（1） It is shown that the OHD can give more stringent constraints on the interacting dark energy model when combined with SNe,CMB and BAO observations,OHD has the potential to alleviate coincidence problem.（2） The special case（＋3wx,corresponding to the LCDM model with no interaction） is within 1σ confidence level with the OHD＋CMB＋BAO,SNe＋CMB＋BAO,and OHD＋ SNe＋CMB＋BAO combinations.