New early dark energy is compatible with current LSS data

Abstract

Recently, a full-shape analysis of large-scale structure (LSS) data was employed to provide new constraints on a class of early dark energy models. In this paper, we derive similar constraints on new early dark energy (NEDE) using the publicly available PyBird code, which makes use of the effective field theory of LSS. We study the NEDE base model with the fraction of NEDE and the trigger field mass as two additional parameters allowed to vary freely, while making simplifying assumptions about the decaying fluid sector. Including the full-shape analysis of LSS together with measurements of the cosmic microwave background, baryonic acoustic oscillations, and supernovae data, we report H 0 ¼ 71.2 AE 1.0 km s −1 Mpc −1 (68% C.L.) together with an approximate 4σ evidence for a nonvanishing fraction of NEDE. This is an insignificant change to the value previously found without full-shape LSS data, H 0 ¼ 71.4 AE 1.0 km s −1 Mpc −1 (68% C.L.). As a result, while the NEDE fit cannot be improved upon the inclusion of additional LSS data, it is also not adversely affected by it, making it compatible with current constraints from LSS data. In fact, we find evidence that the effective field theory of LSS acts in favor of NEDE.

BOSS Correlation Function Analysis from the Effective Field Theory of Large-Scale Structure

“…In particular, the measurements of the Hubble constant represent a novel, CMB-independent, way of determining this parameter [1], which is already comparable in precision with the measurements obtained from the cosmic ladder [8]. In fact, very recently, this capability has been employed to show how some models that were proposed to alleviate the discrepancy between the CMB and cosmic-ladder measurements of the Hubble constant (the so called Hubble tension [9]) do not actually significantly improve the concordance once the BOSS data are analyzed with a controlled model such as the EFTofLSS [10,11] (see also [12,13]).…”

“…where µ = q • ẑ/q, q = q 1 + • • • + q n , and µ i 1 ...in = q i 1 ...in • ẑ/q i 1 ...in , q i 1 ...im = q i 1 + • • • + q im , with ẑ being the unit vector in the direction of the line of sight, f is the growth rate, and n is the order of the kernel Z n . G i are the standard perturbation theory velocity kernels, while K i are the galaxy density kernels given by 12 :…”

Limits on primordial non-Gaussianities from BOSS galaxy-clustering data

“…Such a tool has allowed us to shed much light on how some models that were proposed to alleviate the tension in the Hubble measurements (see e.g. [16]) between the CMB and cosmic ladder [17,18] (see also [19,20]).…”

The Microphysics of Early Dark Energy

“…Early Dark Energy (EDE) has proven to be one of the most promising classes of early-universe solutions, with many models significantly reducing the H 0 tension, while * vivian.i.sabla.gr@dartmouth.edu yielding a comparable fit to the observational data compared to ΛCDM [22][23][24][25][26][27][28][29][30][31][32][33][34][35][36][37][38]. A leading example is standard EDE, consisting of a scalar field that briefly bumps up the expansion rate between equality and recombination.…”