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Quantifying Scalar Field Dynamics with DESI 2024 Y1 BAO measurements
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abstract
Quintessence scalar fields are a natural candidate for evolving dark energy. Unlike the phenomenological $w_0w_a$ parameterization of the dark energy equation of state, they cannot accommodate the phantom regime of dark energy $w(z) < -1$, or crossings into the phantom regime. Recent baryon acoustic oscillation (BAO) measurements by the Dark Energy Spectroscopic Instrument (DESI) indicate a preference for evolving dark energy over a cosmological constant, ranging from $2.6\sigma-3.9\sigma$ when fitting to $w_0w_a$, and combining the DESI BAO measurements with other cosmological probes. In this work, we directly fit three simple scalar field models to the DESI BAO data, combined with cosmic microwave background anisotropy measurements and supernova data sets. We find the best fit model to include a $2-4\%$ kinetic scalar field energy $\Omega_{\rm scf,k}$, for a canonical scalar field with a quadratic or linear potential. However, only the DESY-Y5 supernova data set combination shows a preference for quintessence over $\Lambda$CDM at the $95\%$ confidence level. Fitting to the supernova data sets Pantheon, Pantheon+, DES-Y5, and Union3, we show that the mild tension ($n_{\sigma}< 3.4 $) under $\Lambda$CDM emerges from a BAO preference for smaller values of fractional mass-energy density $\Omega_m < 0.29$, while all supernova data sets, except for Pantheon, prefer larger values, $\Omega_m > 0.3$. The tension under $\Lambda$CDM remains noticeable ($n_{\sigma} <2.8$), when replacing two of the DESI BAO redshift bins with effective redshifts $z_{\text{eff}} =0.51$, and $z_{\text{eff}}= 0.706$ with comparable BOSS DR 12 BAO measurements at $z_{\text{eff}} =0.51$, and $z_{\text{eff}}= 0.61$. Canonical scalar fields as dark energy are successful in mitigating that tension.
Forward citations
Cited by 7 Pith papers
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Bayesian and frequentist perspectives agree on dynamical dark energy
Frequentist profile-likelihood constraints on the CPL dark-energy parameters w0 and wa agree with Bayesian posteriors across DESI, CMB, and SN datasets, corroborating the evidence for dynamical dark energy.
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Robustness of dark energy phenomenology across different parameterizations
The viability of minimally and non-minimally coupled quintessence models is robust across CPL, JBP, BA, and EXP parameterizations, with all four reproducing the models' predicted observables accurately.
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The DESI DR1/DR2 evidence for dynamical dark energy is biased by low-redshift supernovae
The DESI dynamical dark energy preference drops below 2 sigma after correcting a 0.043 mag intercept discrepancy in the low-redshift supernovae of DESY5.
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Is excess smoothing of Planck CMB ansiotropy data partially responsible for evidence for dark energy dynamics in other $w(z)$CDM parametrizations?
In three new w(z)CDM parametrizations, Planck CMB plus non-CMB data favor evolving dark energy over a cosmological constant at roughly 2 sigma when the Planck lensing anomaly parameter is fixed, and at roughly 1 sigma...
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The Status of Single Scalar Field Dark Energy
Cosmological data can constrain only a handful of EFT parameters for single-scalar dark energy; extended models show modest preference over Λ but remain underdetermined and challenged by fifth forces and screening.
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Observational constraints on early time non-phantom behaviour of dynamical dark energy
Early scaling dark energy is constrained to be less than about one percent at matter-radiation equality and is disfavored by model selection, while late-time CPL dynamics show only a weak preference away from ΛCDM.
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Dark energy and lensing anomaly in Planck CMB data
When the Planck lensing amplitude AL is fitted freely, DESI+CMB+SN data no longer prefer evolving dark energy, and DESI BAO's lower matter density worsens the lensing anomaly in LambdaCDM.
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