Observational constraints on a variable dark energy model
Observational constraints on a variable dark energy model
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DOI：
10.1103/physrevd.73.083518
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发表时间：
2005-09
影响因子：
5
通讯作者：
M. Movahed;S. Rahvar
中科院分区：
文献类型：
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作者：
M. Movahed;S. Rahvar
我们研究现象学参数化精华模型对低、中和高红移观测的影响。在低红移和中红移时，我们使用超新星Ia型（SNIa）数据的黄金样本和最近从斯隆数字巡天（SDSS）观测到的重子声波峰的大小，对精华模型的参数进行约束。在高红移处，使用 WAMP 数据完成相同的拟合过程，将声波峰的位置与从暗能量模型获得的位置进行比较。作为平坦宇宙中的补充分析，我们结合了 SNIa、CMB 和 SDSS 的结果。模型参数的最佳拟合值为 ${\ensuremath{\Omega}}_{m}={0.27}_{\ensuremath{-}0.02}^{+0.02}$（当前物质含量）和 ${w}_{0}=\ensuremath{-}{1.45}_{\ensuremath{-}0.60}^{+0.35}$（暗能量方程状态）。最后我们计算这个模型中宇宙的年龄，并将其与老恒星和高红移天体的年龄进行比较。
We study the effect of a phenomenological parameterized quintessence model on low, intermediate and high redshift observations. At low and intermediate redshifts, we use the Gold sample of supernova Type Ia (SNIa) data and recently observed size of baryonic acoustic peak from Sloan Digital Sky Survey (SDSS), to put constraint on the parameters of the quintessence model. At the high redshift, the same fitting procedure is done using WAMP data, comparing the location of acoustic peak with that obtain from the dark energy model. As a complementary analysis in a flat universe, we combine the results from the SNIa, CMB and SDSS. The best fit values for the model parameters are ${\ensuremath{\Omega}}_{m}={0.27}_{\ensuremath{-}0.02}^{+0.02}$ (the present matter content) and ${w}_{0}=\ensuremath{-}{1.45}_{\ensuremath{-}0.60}^{+0.35}$ (dark energy equation of state). Finally we calculate the age of universe in this model and compare it with the age of old stars and high redshift objects.