Cosmological constraints from the power spectrum of eBOSS emission line galaxies

TL;DR

This paper uses the power spectrum of emission line galaxies from eBOSS to measure cosmological parameters within the $ u\Lambda$CDM model, highlighting the impact of non-linear redshift-space distortions and comparing results with CMB data.

Contribution

It provides the first detailed analysis of ELG power spectrum with effective field theory, including non-linear distortions, and offers updated cosmological constraints from eBOSS data.

Findings

Constraints on $\Omega_m$, $\sigma_8$, and $H_0$ from ELG data

Neural redshift-space distortions are weaker than in luminous red galaxies

A $\sim 3σ$ tension in clustering amplitude with CMB data

Abstract

We present cosmological parameter measurements from the effective field theory-based full-shape analysis of the power spectrum of emission line galaxies (ELGs). First, we perform extensive tests on simulations and determine appropriate scale cuts for the perturbative description of the ELG power spectrum. We study in detail non-linear redshift-space distortions (``fingers-of-God'') for this sample and show that they are somewhat weaker than those of luminous red galaxies. This difference is not significant for current data, but may become important for future surveys like Euclid/DESI. Then we analyze recent measurements of the ELG power spectrum from the extended Baryon acoustic Oscillation Spectroscopic Survey (eBOSS) within the $\nu\Lambda$CDM model. Combined with the BBN baryon density prior, the ELG pre- and post-reconstructed power spectra alone constrain the matter density $\Omega_m=0.257_{-0.045}^{+0.031}$, the current mass fluctuation amplitude $\sigma_8=0.571_{-0.076}^{+0.052}$, and the Hubble constant $H_0=84.5_{-7}^{+5.8}$ km/s/Mpc (all at 68\% CL). Combining with other full-shape and BAO data we measure $\Omega_m=0.327_{-0.016}^{+0.014}$, $\sigma_8=0.69_{-0.045}^{+0.038}$, and $H_0=68.6_{-1.1}^{+1}$ km/s/Mpc. The total neutrino mass is constrained to be $M_{\rm tot}<0.63$ eV (95\% CL) from the BBN, full-shape and BAO data only. Finally, we discuss the apparent $\sim 3\sigma$ discrepancy in the inferred clustering amplitude between our full shape analysis and the cosmic microwave background data.