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Calibrating Dark Energy

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arxiv 0808.0189 v1 pith:E4G5MCLB submitted 2008-08-01 astro-ph

Calibrating Dark Energy

Roland de Putter , Eric V. Linder This is my paper
classification astro-ph
keywords darkenergycalibrationfactorparameterrelationtimevariation
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved
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Exploring the diversity of dark energy dynamics, we discover a calibration relation, a uniform stretching of the amplitude of the equation of state time variation with scale factor. This defines homogeneous families of dark energy physics. The calibration factor has a close relation to the standard time variation parameter w_a, and we show that the new, calibrated w_a describes observables, i.e. distance and Hubble parameter as a function of redshift, typically to an accuracy level of 10^{-3}. We discuss implications for figures of merit for dark energy science programs.

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Cited by 6 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. DESI DR2 Results II: Measurements of Baryon Acoustic Oscillations and Cosmological Constraints

    astro-ph.CO 2025-03 accept novelty 7.0

    DESI DR2 BAO data exhibits 2.3 sigma tension with CMB in Lambda-CDM but prefers evolving dark energy (w0 > -1, wa < 0) at 3.1 sigma with CMB and 2.8-4.2 sigma when including supernovae.

  2. DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations

    astro-ph.CO 2024-04 accept novelty 7.0

    First-year DESI BAO data are consistent with flat LambdaCDM and, when combined with CMB, show a 2.5-3.9 sigma preference for evolving dark energy (w0 > -1, wa < 0) that strengthens with certain supernova datasets.

  3. Assessing observational constraints on dark energy

    astro-ph.CO 2024-05 conditional novelty 6.0

    Quintessence models satisfying NEC everywhere predict the w0 > -1 and w0+wa < -1 sector favored by data, due to an approximate degeneracy in the w(z) = w0 + wa z/(1+z) parameterization.

  4. Disentangling cosmic distance tensions with early and late dark energy

    astro-ph.CO 2026-04 unverdicted novelty 5.0

    Early dark energy resolves CMB-BAO tension and, combined with thawing quintessence, reduces overall cosmological tensions without phantom crossing.

  5. Reanalyzing DESI DR1: 2. Constraints on Dark Energy, Spatial Curvature, and Neutrino Masses

    astro-ph.CO 2025-11 unverdicted novelty 5.0

    Reanalysis of DESI full-shape clustering data tightens constraints on neutrino mass, spatial curvature, and dark energy equation-of-state parameters relative to BAO-only results.

  6. Extended Dark Energy analysis using DESI DR2 BAO measurements

    astro-ph.CO 2025-03 conditional novelty 4.0

    Extended analysis of DESI DR2 data confirms robust evidence for dynamical dark energy with phantom crossing preference, stable under parametric and non-parametric modeling.