Papers › Quantifying Scalar Field Dynamics with DESI 2024 Y1 BAO measurements
Quantifying Scalar Field Dynamics with DESI 2024 Y1 BAO measurements
Kim V. Berghaus, Joshua A. Kable, Vivian Miranda
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Quintessence scalar fields are a natural candidate for evolving dark energy. Unlike the phenomenological w₀wₐ 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 2.6σ-3.9σ when fitting to w₀wₐ, 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 Ω_(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 ΛCDM at the 95% confidence level. Fitting to the supernova data sets Pantheon, Pantheon+, DES-Y5, and Union3, we show that the mild tension (n_σ< 3.4) under ΛCDM emerges from a BAO preference for smaller values of fractional mass-energy density Ωₘ < 0.29, while all supernova data sets, except for Pantheon, prefer larger values, Ωₘ > 0.3. The tension under ΛCDM remains noticeable (n_σ <2.8), when replacing two of the DESI BAO redshift bins with effective redshifts z_(eff) =0.51, and z_(eff)= 0.706 with comparable BOSS DR 12 BAO measurements at z_(eff) =0.51, and z_(eff)= 0.61. Canonical scalar fields as dark energy are successful in mitigating that tension.
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