New tests of dark sector interactions from the full-shape galaxy power spectrum

Rafael C. Nunes, Sunny Vagnozzi, Suresh Kumar, Eleonora Di Valentino, and Olga Mena

Phys. Rev. D 105, 123506 – Published 8 June 2022

Abstract

We explore the role of redshift-space galaxy clustering data in constraining nongravitational interactions between dark energy (DE) and dark matter (DM), for which state-of-the-art limits have so far been obtained from late-time background measurements. We use the joint likelihood for prereconstruction full-shape (FS) galaxy power spectrum and postreconstruction Baryon Acoustic Oscillation (BAO) measurements from the BOSS DR12 sample, alongside Cosmic Microwave Background (CMB) data from Planck: from this dataset combination we infer $H_{0} = 68.0 2_{- 0.60}^{+ 0.49} km / s / Mpc$ and the $2 σ$ lower limit $ξ > - 0.12$ , among the strongest limits ever reported on the DM-DE coupling strength $ξ$ for the particular model considered. Contrary to what has been observed for the $Λ CDM$ model and simple extensions thereof, we find that the $CMB + FS$ combination returns tighter constraints compared to the $CMB + BAO$ one, suggesting that there is valuable additional information contained in the broadband of the power spectrum. We test this finding by running additional CMB-free analyses and removing sound horizon information, and discuss the important role of the equality scale in setting constraints on DM-DE interactions. Our results reinforce the critical role played by redshift-space galaxy clustering measurements in the epoch of precision cosmology, particularly in relation to tests of nonminimal dark sector extensions of the $Λ CDM$ model.

Received 18 March 2022
Accepted 19 May 2022

DOI:https://doi.org/10.1103/PhysRevD.105.123506

Physics Subject Headings (PhySH)

Cosmology Dark energy Dark matter

Gravitation, Cosmology & Astrophysics

Authors & Affiliations

Rafael C. Nunes ^1,2,*, Sunny Vagnozzi ^3,†, Suresh Kumar ^4,‡, Eleonora Di Valentino ^5,§, and Olga Mena^6,∥

¹Instituto de Física, Universidade Federal do Rio Grande do Sul, 91501-970 Porto Alegre RS, Brazil
²Divisão de Astrofísica, Instituto Nacional de Pesquisas Espaciais, Avenida dos Astronautas 1758, São José dos Campos, 12227-010 São Paulo, Brazil
³Kavli Institute for Cosmology (KICC) and Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, United Kingdom
⁴Department of Mathematics, Indira Gandhi University, Meerpur, Haryana 122502, India
⁵School of Mathematics and Statistics, University of Sheffield, Hounsfield Road, Sheffield S3 7RH, United Kingdom
⁶Instituto de Física Corpuscular (IFIC), University of Valencia-CSIC, E-46980 Valencia, Spain

^*rafadcnunes@gmail.com
^†sunny.vagnozzi@ast.cam.ac.uk
^‡suresh.math@igu.ac.in
^§e.divalentino@sheffield.ac.uk
^∥omena@ific.uv.es

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Vol. 105, Iss. 12 — 15 June 2022

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Images

Figure 1
Left: measurements of the monopole ( $ℓ = 0$ ) and quadrupole ( $ℓ = 2$ ) of the full-shape power spectrum of the BOSS DR12 North galactic cap galaxy field at the effective redshift $z_{eff} = 0.61$ correspond to the black datapoints. The blue and red curves correspond to the theoretical predictions for the monopole and quadrupole respectively, for the $Λ CDM$ (solid) and IDE (dashed) models. Cosmological parameters are fixed to their best-fit values obtained from the $CMB + BAO + FS$ dataset combination (see Sec. 3 for a discussion of these datasets), with the DM-DE coupling strength $ξ$ instead being fixed to $ξ = - 0.05$ , whereas nuisance parameters are fixed to their $Λ CDM$ best-fit values. Note that for both the monopole and quadrupole what is being plotted is not $P_{ℓ} (k)$ , but $k P_{ℓ} (k)$ . Right: relative difference $Δ P_{ℓ} / P_{ℓ}$ between the IDE and $Λ CDM$ monopole (blue) and quadrupole (red), with the same choice of cosmological and nuisance parameters as in the left panel.
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Figure 2
Triangular plot showing the 2D joint and 1D marginalized posterior probability distributions for $ξ$ , $Ω_{m}$ , and $H_{0}$ , obtained from the $CMB + BAO$ (grey), $CMB + FS$ (red), and $CMB + BAO + FS$ (blue) dataset combinations within the IDE model. The significant improvement in constraining power gained by the introduction of the FS dataset is visually very clear. Note that $H_{0}$ is in units of $km / s / Mpc$ .
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Figure 3
Left: 1D marginalized posterior probability distributions for $H_{0}$ , obtained from various dataset combinations (see the color coding) within the IDE model. The pink-shaded band corresponds to the $1 σ$ credible region for $H_{0}$ determined by the latest local distance ladder measurements constructed out of Cepheid-calibrated SNeIa [324]. Right: 1D marginalized posterior probability distributions for $H_{0}$ , obtained from the $CMB + BAO$ and $CMB + BAO + FS$ dataset combination within the $Λ CDM$ (green and red curves, respectively) and IDE (blue and black curves, respectively) models. From this figure it is clear that there is a significant gain in constraining power within the IDE model when including the FS dataset, contrary to what is observed within $Λ CDM$ . The pink-shaded band is equivalent to that depicted in the left panel.
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Figure 4
As Fig. 2, but considering dataset combinations not involving the CMB dataset: $FS + BAO$ (red) and $FS + BAO + BBN$ (blue). It is clear that the inclusion of the BBN prior on $ω_{b}$ helps enormously with the determination of $H_{0}$ , given that current galaxy clustering data mainly constrain $H_{0}$ through the sound horizon rather than through equality-scale information (with the prior on $ω_{b}$ sharpening the former), as discussed in the main text.
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Physical Review D

covering particles, fields, gravitation, and cosmology