Early dark energy cosmologies

By M. Doran, G. Robbers. 2006

189 citations recorded by the source corpus.

We propose a novel parameterization of the dark energy density. It is particularly well suited to describe a non-negligible contribution of dark energy at early times and contains only three parameters, which are all physically meaningful: the fractional dark energy density today, the equation of state today and the fractional dark energy density at early times. As we parameterize Ωd(a) directly instead of the equation of state, we can give analytic expressions for the Hubble parameter, the conformal horizon today and at last scattering, the sound horizon at last scattering, and the acoustic scale as well as the luminosity distance. For an equation of state today w0<−1, our model crosses the cosmological constant boundary. We perform numerical studies to constrain the parameters of our model by using cosmic microwave background (CMB), large scale structure (LSS) and supernovae Ia (SNe Ia) data. At 95% confidence, we find that the fractional dark energy density at early times Ωde<0.06. This bound tightens considerably to Ωde<0.04 when the latest Boomerang data are included. We find that both the gold sample of Riess et al and the SNLS data of Astier et al when combined with CMB and LSS data mildly prefer w0<−1, but are well compatible with a cosmological constant.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c41dd8059759977537a80c444e2a8d61077aa811

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Citations in the corpus

The Atacama Cosmology Telescope: cosmological parameters from three seasons of data (2013, unknown): “(1988); Doran & Robbers (2006) d ln a + a eq 3( a + a eq ) .”
The Ups and Downs of Early Dark Energy solutions to the Hubble tension: A review of models, hints and constraints circa 2023 (2023, background): “[73] Michael Doran and Georg Robbers, “Early dark energy cosmologies,” JCAP 06, 026 (2006), arXiv:astro-ph/0601544.”
Maximal freedom at minimum cost: linear large-scale structure in general modifications of gravity (2014, unknown): “[92].”
Vector field models of inflation and dark energy (2008, background): “3) In addition, the possibility of early dark energy, which the scaling solutions automatically incorporate, is phenomenologically interesting [55].”
Measurement of baryon acoustic oscillations in the Lyman-α forest fluctuations in BOSS data release 9 (2013, background): “Dark energy suffers from many tuning problems that can be alleviated by introducing an early dark energy component [11–16].”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Measuring growth rate and geometry with anisotropic clustering (2013, background): “(For DE models that do not belong to this family see e.g. Wetterich 2004; Doran & Robbers 2006).”
Extragalactic science, cosmology, and Galactic archaeology with the Subaru Prime Focus Spectrograph (2012, methodology): “For comparison, the dashed curve shows the dark energy density parameter for an early dark energy (EDE) model proposed in Doran & Robbers (2006), which gives a more significant contribution to the cosmic expansion at higher redshift than in the cosmological constant: ΩEDEde (a) = Ωde0 − Ωe(1 −…”
CONSTRAINTS ON COSMOLOGY FROM THE COSMIC MICROWAVE BACKGROUND POWER SPECTRUM OF THE 2500 deg2 SPT-SZ SURVEY (2012, methodology): “Instead of considering a specific model, we choose to constrain early dark energy in the more general tracer model parametrization by Doran & Robbers (2006).”
The DESI Experiment Part I: Science,Targeting, and Survey Design (2016, background): “An interesting possibility is that dark energy density does not become completely negligible at high redshift, as predicted by the cosmological constant or other models with w ' −1, but rather remains at a level predicted by some particle-physics models and detectable by future surveys [30, 31, 32, ”