Supernova data may be unable to distinguish between quintessence and k-essence

Abstract

We consider the efficacy of using luminosity distance measurements of deep redshift supernovae to discriminate between two forms of dark energy, quintessence (a scalar field with canonical kinetic terms rolling down a potential) and k-essence (a scalar field whose cosmic evolution is driven entirely by non-linear kinetic terms). The primary phenomenological distinction between the two types of models that can be quantified by supernova searches (at least in principle) is that the equation of state $w\equiv p/\rho$ of quintessence is falling today while that of k-essence is rising. By simulating $10^5$ possible datasets that SNAP could obtain, we show that even if the mass density ${\Omega }_m$ is known exactly, an ambiguity remains that may not allow a definitive distinction to be made between the two types of theories.

Version to appear in PLB

References in corpus (10)

• A Flat Universe from High-Resolution Maps of the Cosmic Microwave Background Radiation
• k-Inflation
• Kinetically Driven Quintessence
• The Cosmic Triangle: Revealing the State of the Universe
• Quintessence arising from exponential potentials
• Reconstructing the Cosmic Equation of State from Supernova distances
• Quintessence and Supergravity
• Phenomenology of a realistic accelerating universe using only Planck-scale physics
• Constraining the equation of state of the Universe from Distant Type Ia Supernovae and Cosmic Microwave Background Anisotropies
• Supernovae Ia Constraints on a Time-Variable Cosmological "Constant"

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• Measuring the Equation-of-state of the Universe: Pitfalls and Prospects
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• Model-Independent Constraints on Dark Energy Density from Flux-averaging Analysis of Type Ia Supernova Data
• A model independent approach to the dark energy equation of state
• Future supernovae data and quintessence models
• Direct Determination of the Kinematics of the Universe and Properties of the Dark Energy as Functions of Redshift
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• Prospects for Determining the Equation of State of the Dark Energy: What can be Learned from Multiple Observables?
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• Future Type Ia Supernova Data as Tests of Dark Energy from Modified Friedmann Equations
• Binned Cosmic Microwave Background Anisotropy Power Spectra: Peak Location
• Probing Dark Energy Using Its Density Instead of Its Equation of State
• SO(1,1) dark energy model and the universe transition
• Dark Energy in Practice
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• Quintessence Cosmology and the Cosmic Coincidence
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• Unbiased Estimate of Dark Energy Density from Type Ia Supernova Data
• Analysis of two quintessence models with SN Ia data
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