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Features of holographic dark energy under combined cosmological constraints

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Abstract

We investigate the observational signatures of the holographic dark-energy models, including both the original model and a model with an interaction term between the dark energy and dark matter. We first delineate the dynamical behavior of such models, especially considering whether they would have a “big rip” for different parameters; then we use several recent observations, including 182 high-quality type Ia supernovae data observed with the Hubble Space Telescope, the SNLS and ESSENCE surveys, 42 latest Chandra X-ray cluster gas mass fraction, 27 high-redshift gamma-ray burst samples, the baryon acoustic oscillation measurement from the Sloan Digital Sky Survey, and the CMB shift parameter from the WMAP three-year result to give more reliable and tighter constraints on the holographic dark-energy models. The results of our constraints for the holographic dark-energy model without interaction is c=0.748 +0.108−0.009 , Ω m0=0.276 +0.017−0.016 , and for the model with interaction (c=0.692 +0.135−0.107 , Ω m0=0.281 +0.017−0.017 , α=−0.006 +0.021−0.024 , where α is an interacting parameter). As these models have more parameters than the ΛCDM model, we use the Bayesian Evidence as a model-selection criterion to make comparisons. We found that the holographic dark-energy models are mildly favored by the observations as compared to the ΛCDM model.

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Authors and Affiliations

  1. Kavli Institute for Theoretical Physics China, Institute of Theoretical Physics, Chinese Academy of Sciences, P.O. Box 2735, Beijing, 100080, China

    Yin-Zhe Ma & Xuelei Chen

  2. Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK

    Yin-Zhe Ma

  3. National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, China

    Yan Gong & Xuelei Chen

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  1. Yin-Zhe Ma
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Ma, YZ., Gong, Y. & Chen, X. Features of holographic dark energy under combined cosmological constraints. Eur. Phys. J. C 60, 303–315 (2009). https://doi.org/10.1140/epjc/s10052-009-0876-7

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