ACCELERATING UNIVERSES WITH SCALING DARK MATTER

By M. Chevallier, D. Polarski. 2000

1,970 citations recorded by the source corpus.

Friedmann–Robertson–Walker universes with a presently large fraction of the energy density stored in an X-component with wX<-1/3, are considered. We find all the critical points of the system for constant equations of state in that range. We consider further several background quantities that can distinguish the models with different wX values. Using a simple toy model with a varying equation of state, we show that even a large variation of wX at small redshifts is very difficult to observe with dL(z) measurements up to z~1. Therefore, it will require accurate measurements in the range 1<z<2 and independent accurate knowledge of Ωm,0 (and/or ΩX,0) in order to resolve a variable wX from a constant wX.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/6df606f8dca5e76811cd246b8afa17905c0662b9

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Citations in the corpus

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Measuring growth rate and geometry with anisotropic clustering (2013, background): “…a wide range of DE models that do not exhibit sudden transitions or large amount of DE at early times, for example models based on cosmological scalar fields, this time-dependence can be adequately parametrized by two parameters w(z) = w0 + wa z 1 + z (32) (Chevallier & Polarski 2001; Linder 2003).”
hi_class: Horndeski in the Cosmic Linear Anisotropy Solving System (2016, background): “wowa: evolving equation of state with parameters (ΩDE,0, w0, wa) [81, 82] with the constraint that the density fraction today satisfies the closure relation (3.”
MEASURING BARYON ACOUSTIC OSCILLATIONS ALONG THE LINE OF SIGHT WITH PHOTOMETRIC REDSHIFTS: THE PAU SURVEY (2008, methodology): “In the following, we will be using the standard parametrization (Chevallier & Polarski 2001; Linder 2003) of the time evolution of the DE equation of state, w(z) = w0 +wa · (1−a), where w0 denotes the equation of state now, and wa is (minus) its current derivative with respect to the scale factor a.”
Distance priors from Planck final release (2018, methodology): “In this section, we use the distance priors derived for the base ΛCDM model in the former subsection to constrain the cosmological parameters in the base ΛCDM model, the wCDM model and the CPL model [28, 29], and compare our results with the Planck 2018 results to test the validity of the distance p”
SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2010, methodology): “Time-dependent Equation of State As for a time-dependent equation of state, we shall find constraints on the present-day value of the equation of state and its derivative using a linear form, w(a) = w0 + wa(1−a) (Chevallier & Polarski 2001; Linder 2003).”
NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL PARAMETER RESULTS (2012, neutral): “21 When w is allowed to vary with the scale factor according to w(a) = w0 + wa(1 − a) (Chevallier & Polarski 2001; Linder 2003), we find, for a flat universe20 4.6.1.”
The clustering of galaxies in the SDSS‐III Baryon Oscillation Spectroscopic Survey: cosmological implications of the large‐scale two‐point correlation function (2012, methodology): “In Section 5.5.2 we allow also for a time variation of this parameter using the standard linear parametrization of Chevallier & Polarski (2001) and Linder (2003) given by wDE(a) = w0 + wa(1− a), (12) 2 When including tensor modes we assume the slow-roll consistency relation and fix the tensor…”
KiDS-450: testing extensions to the standard cosmological model (2016, background): “…form of a first-order Taylor expansion with two free parameters: w(a) = w0 + (1 − a)wa, (5) where a is the cosmic scalefactor, w0 is the dark energy equation of state at present and wa = −dw/da|a = 1 (which can also be expressed as wa = −2dw/d ln a|a = 1/2; Chevallier & Polarski 2001; Linder 2003).”
Nonlocal gravity. Conceptual aspects and cosmological predictions (2017, methodology): “Comparing with the commonly used parametrization of the form [91, 92]”