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Exploring the Expansion History of the Universe
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Exploring the Expansion History of the Universe
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Exploring the recent expansion history of the universe promises insights into the cosmological model, the nature of dark energy, and potentially clues to high energy physics theories and gravitation. We examine the extent to which precision distance-redshift observations can map out the history, including the acceleration-deceleration transition, and the components and equations of state of the energy density. We consider the ability to distinguish between various dynamical scalar field models for the dark energy, as well as higher dimension and alternate gravity theories. Finally, we present a new, advantageous parametrization for the study of dark energy.
Forward citations
Cited by 60 Pith papers
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DESI 2024 VII: Cosmological Constraints from the Full-Shape Modeling of Clustering Measurements
DESI DR1 full-shape clustering yields Ω_m = 0.2962 ± 0.0095 and σ_8 = 0.842 ± 0.034 in flat ΛCDM, tightening to H_0 = 68.40 ± 0.27 km/s/Mpc with CMB and DESY3, while favoring w_0 > -1, w_a < 0 and limiting neutrino ma...
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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.
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Growth, geometry, and early-universe split of the matter density parameter $\Omega_{\rm m}$
Splitting Ω_m into geometry, growth, and early-universe regimes yields mutually compatible values, yet ΔΩ_m^{geo,early} is 2σ from zero under combined DES, Planck (scale-cut), DESI, Pantheon+, and RSD data.
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EFT-Ramses: a code to simulate the effective field theory of dark energy
A unified AMR N-body code embeds EFTofDE α-basis models into one master Vainshtein equation and matches legacy ECOSMOG and HiCOLA matter power spectra.
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Constraints on Horndeski Gravity with Phantom Crossing
Asymptotic Cubic Galileon models can fit Planck+DESI+DES expansion history with phantom crossing and are tightly constrained by galaxy-ISW and void-force observables.
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Exploring the interplay of late-time dynamical dark energy and new physics before recombination
Under standard recombination, phantom-crossing dynamical dark energy is preferred at ~97–98.5% probability; early-time fixes to the Hubble tension erase that preference while creating severe ω_m tension with CMB.
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Signatures of kinetic gravity braiding in cosmological probes of the gravitational field
KGB braiding boosts weak-lensing power by ~10–12% at ℓ~10²–10³ and flips the ISW–RS difference from suppression to excess once nonlinear Rees–Sciama physics dominates.
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Late-Time Cosmological Tests of a Minisuperspace Generalized-Uncertainty-Principle Deformation
Fitting a GUP-deformed Friedmann equation to CC+Pantheon++DESI DR2 data gives β* = −0.086 with a 95% interval including zero; the negative preference vanishes under stricter perturbative cuts.
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Can cosmic voids ease the Hubble tension? Local expansion in $w_0w_a$CDM
A KBC-like local void lowers the SH0ES–Planck Hubble tension to about 2σ but cannot fully resolve it, and evolving dark energy shifts the required void depth by only ~1%.
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The Goldstone Awakens: Unimodular dark energy in scale-invariant $R^2$ gravity
In a scale-invariant R² + unimodular-gravity model, the Goldstone boson of scale symmetry becomes thawing dark energy, with its equation of state fixed by the same coupling that sets the inflationary spectral tilt.
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Phantom crossing from the Standard Model and General Relativity
Fermion-condensate vacuum energy plus Buchert backreaction from nonlinear structure formation yields a low-redshift phantom crossing consistent with DESI+CMB+SNIa data for a chosen backreaction density.
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A hybrid method for reconstruction of the equation of state of dark energy and its application to Pantheon+SH0ES data
Hybrid semi-parametric reconstruction of dark energy equation of state from distance-redshift data applied to Pantheon+SH0ES yields results consistent with w = -1.
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Are Cosmological Data Excluding Sterile Neutrinos or Only the Fully Thermalized Limit?
Cosmological observations constrain the effective abundance of light sterile neutrinos tightly while allowing non-fully-thermalized realizations to remain viable across LambdaCDM and CPL models.
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Evolving Dark Energy Is Vacuum Energy After All
A QCD-vacuum dark-energy model with a two-parameter switch reproduces the DESI-preferred late-time expansion and is mildly favoured over ΛCDM by Bayesian evidence (lnB≈2.7).
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Constraints on the Sum of Neutrino Masses from ACT DR6 and DESI DR2 Considering Isocurvature Initial Conditions
Including neutrino density isocurvature in fits to ACT DR6, DESI DR2, and DES data yields ∑m_ν < 0.057 eV at 95% CL in ΛCDM with no detection of the isocurvature mode.
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Bounding the Effect of HOD Assumptions on Small-Scale Clustering Constraints
The fraction of AbacusSummit cosmologies excluded at 3σ by small-scale clustering multipoles drops from 81% to 25% when moving from fixed HOD parameters to broad marginalization over the five-parameter HOD model.
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The DESI results impact the local determination of $H_0$
Reanalysis shows DESI-preferred w0wa models reduce local H0 by 0.5-2.5 km s^{-1} Mpc^{-1} relative to LambdaCDM.
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Dissipative Dark Energy can explain the DESI phantom crossing
Weakly dissipative quintessence explains DESI phantom crossing in dark energy without pathological dynamics.
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Constraints on the gravitational potential from DESI DR2 BAO and its implications for the local void scenario
High-redshift datasets constrain the local void gravitational redshift parameter z0 to be consistent with zero but allow the value needed for Hubble tension solution.
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