A new determination of the primordial helium abundance using the analyses of HII region spectra from SDSS

TL;DR

This study measures the primordial helium abundance using SDSS HII region spectra, providing a precise value consistent with Planck results, and constrains the effective number of neutrino species.

Contribution

It presents a new, self-consistent analysis of 100 HII regions from SDSS to determine the primordial helium abundance with high precision.

Findings

Primordial helium abundance Yp = 0.2462 ± 0.0022.

Effective neutrino number Neff = 2.95 ± 0.16.

Results agree with Planck cosmological measurements.

Abstract

The precision measurement of the primordial helium abundance $Y_p$ is a powerful probe of the early Universe. The most common way to determine $Y_p$ is analyses of observations of metal-poor \HII regions found in blue compact dwarf galaxies. We present the spectroscopic sample of 100 \HII regions collected from the Sloan Digital Sky Survey. The final analysed sample consists of our sample and HeBCD database from Izotov et al. 2007. We use a self-consistent procedure to determine physical conditions, current helium abundances, and metallicities of the \HII regions. From a regression to zero metallicity, we have obtained $Y_p = 0.2462 \pm 0.0022$ which is one of the most stringent constraints obtained with such methods up to date and is in a good agreement with the Planck result $Y_{\rm p}^{\it {Planck}} = 0.2471 \pm 0.0003$. Using the determined value of $Y_p$ and the primordial deuterium abundance taken from Particle Data Group (Zyla et al. 2020) we put a constraint on the effective number of neutrino species $N_{\rm eff} = 2.95 \pm 0.16$ which is consistent with the Planck one $N_{\rm eff} = 2.99 \pm 0.17$. Further increase of statistics potentially allows us to achieve Planck accuracy, which in turn will become a powerful tool for studying the self-consistency of the Standard Cosmological Model and/or physics beyond.