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

Abstract

We explore the role of redshift-space galaxy clustering data in constraining non-gravitational 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 pre-reconstruction full-shape (FS) galaxy power spectrum and post-reconstruction Baryon Acoustic Oscillation (BAO) measurements from the BOSS DR12 sample, alongside Cosmic Microwave Background (CMB) data from Planck : from this dataset combination we infer H0 = 68.02 +0.49 −0.60 km/s/Mpc and the 2σ 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 ΛCDM 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 CMBfree 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 non-minimal dark sector extensions of the ΛCDM model.

Updating non-standard neutrinos properties with Planck-CMB data and full-shape analysis of BOSS and eBOSS galaxies

“…The effective field theory-based full-shape analysis of the power spectrum has been applied to derive constraints on m ν and N eff in [10,[61][62][63]. Also, EFTofLSS has been used to constrain the standard cosmological parameters and models beyond the ΛCDM cosmology (See [62,[64][65][66][67][68][69][70][71][72][73][74][75][76][77][78][79][80][81][82]). Besides the EFTofLSS, a number of other theoretical modeling approaches have been adopted in the analysis for galaxy clustering data to derive constraints on m ν and N eff (see [77,[83][84][85][86][87][88][89][90][91][92][93][94][95][96][97][98] for a short list).…”

Determining the Hubble Constant without the Sound Horizon: A $3.6\%$ Constraint on $H_0$ from Galaxy Surveys, CMB Lensing and Supernovae

“…The first approach was to use the CMB lensing power spectrum [22]; since this observable is given by a projection of the matter power spectrum, the BAO oscillations average out such that only equality scale information remains. Later approaches [23,24] improved upon these constraints with novel analyses of the full 3D galaxy power spectrum, building on recent advances in modeling and analyzing the galaxy power spectrum, beyond just its oscillatory component [e.g., [25][26][27][28][29][30][31][32][33]. Whilst constraints from standard full-shape analyses remain BAOdominated, [24] successfully removed sound horizon information with a suitable choice of priors (omitting the baryonic information usually provided by Big Bang Nucleosynthesis (BBN) constraints [e.g., 13,28,34,35]); subsequently, [23] proposed and validated a new method to "integrate out" the sound horizon even with BBN priors, resulting in the tightest equality scale H 0 constraints to date.…”

Determining the Hubble constant without the sound horizon: A 3.6% constraint on H0 from galaxy surveys, CMB lensing, and supernovae

“…The first approach was to use the CMB lensing power spectrum [24]; since this observable is given by a projection of the matter power spectrum, the BAO oscillations average out such that only equality scale information remains. Later approaches [25,26] improved upon these constraints with novel analyses of the full 3D galaxy power spectrum, building on recent advances in modeling and analyzing the galaxy power spectrum, beyond just its oscillatory component [e.g., [27][28][29][30][31][32][33][34][35]. Whilst constraints from standard fullshape analyses remain BAO-dominated, [26] successfully removed sound horizon information with a suitable choice of priors (omitting the baryonic information usually provided by Big Bang Nucleosynthesis (BBN) constraints [e.g., 15,30,36,37]); subsequently, [25] proposed and validated a new method to "integrate out" the sound horizon even with BBN priors, resulting in the tightest equality scale H 0 constraints to date.…”