H_0 tension in dark energy cosmology
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Date
2018
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Recently, the equation of state on dark energy has dropped lower than the edge of -1. Based on this outcome, the nature of dark energy may be far away from cosmological constant. As the adjustment on the equation of state keeps decreasing, the introduction of phantom seems necessary. By employing the observational constraints on supernovas and the acoustic scale of the cosmic microwave background(CMB), where the accuracy has become extraordinary, we apply a phenomenological method to mimic the evolution of the universe. The demonstration on the constraining evolution of phantom will show the model has high consistency with current observation.
Recently, the equation of state on dark energy has dropped lower than the edge of -1. Based on this outcome, the nature of dark energy may be far away from cosmological constant. As the adjustment on the equation of state keeps decreasing, the introduction of phantom seems necessary. By employing the observational constraints on supernovas and the acoustic scale of the cosmic microwave background(CMB), where the accuracy has become extraordinary, we apply a phenomenological method to mimic the evolution of the universe. The demonstration on the constraining evolution of phantom will show the model has high consistency with current observation.
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Keywords
Dark energy, Hubble constant problem, Dynamically evolving dark energy, quintessence, phantom, Dark energy, Hubble constant problem, Dynamically evolving dark energy, quintessence, phantom