Constraining cosmological scaling solutions of a Galileon field

2021/12/31 by Inês S. Albuquerque, Noemi Frusciante, M. Martinelli +1
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics #Baryon acoustic oscillations #Classical mechanics #Cosmic microwave background #Cosmology #Cosmology and Gravitation Theories #Dark energy #Galaxy #Geophysics and Gravity Measurements #Kinetic term #Matter power spectrum #Phenomenology (philosophy) #Physics #Planck #Pulsars and Gravitational Waves Research #Quantum mechanics #Redshift #Scalar field #Scaling #Theoretical physics #Universality (dynamical systems) #astro-ph.CO #gr-qc

paper · pdf · doi:10.1103/physrevd.105.044056

published in Physical review. D/Physical review. D. 105(4) (American Physical Society) · 12 pages, 9 figures

openalex created_date 2021/12/31 · arxiv created 2022/02/28 · openalex publication_date 2022/02/28 · arxiv updated 2022/03/02 · openalex updated_date 2026/08/05

Abstract

We study a Lagrangian with a cubic Galileon term and a standard scalar-field kinetic contribution with two exponential potentials. In this model the Galileon field generates scaling solutions in which the density of the scalar field ϕ scales in the same manner as the matter density at early-time. These solutions are of high interest because the scalar field can then be compatible with the energy scale of particle physics and can alleviate the coincidence problem. The phenomenology of linear perturbations is thoroughly discussed, including all the relevant effects on the observables. Additionally, we use cosmic microwave background temperature-temperature and lensing power spectra by Planck 2018, the baryon acoustic oscillations measurements from the 6dF galaxy survey and SDSS and supernovae type Ia data from Pantheon in order to place constraints on the parameters of the model. We find that despite its interesting phenomenology, the model we investigate does not produce a better fit to data with respect to ΛCDM, and it does not seem to be able to ease the tension between high and low redshift data.

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