The primordial helium abundance from updated emissivities

TL;DR

This study updates the primordial helium abundance estimate by incorporating new He I emissivities, resulting in a slightly lower Y_p value with larger uncertainties, aligning well with Planck results.

Contribution

It introduces updated atomic emissivities into the analysis, refining the primordial helium abundance measurement with a comprehensive MCMC approach.

Findings

Y_p = 0.2465 +/- 0.0097 from updated data

Good agreement with Planck's Y_p value

Increased uncertainties and variance in measurements

Abstract

Observations of metal-poor extragalactic H II regions allow the determination of the primordial helium abundance, Y_p. The He I emissivities are the foundation of the model of the H II region's emission. Porter, Ferland, Storey, & Detisch (2012) have recently published updated He I emissivities based on improved photoionization cross-sections. We incorporate these new atomic data and update our recent Markov Chain Monte Carlo analysis of the dataset published by Izotov, Thuan, & Stasinska (2007). As before, cuts are made to promote quality and reliability, and only solutions which fit the data within 95% confidence level are used to determine the primordial He abundance. The previously qualifying dataset is almost entirely retained and with strong concordance between the physical parameters. Overall, an upward bias from the new emissivities leads to a decrease in Y_p. In addition, we find a general trend to larger uncertainties in individual objects (due to changes in the emissivities) and an increased variance (due to additional objects included). From a regression to zero metallicity, we determine Y_p = 0.2465 +/- 0.0097, in good agreement with the Planck result of Y_p = 0.2485 +/- 0.0002. In the future, a better understanding of why a large fraction of spectra are not well fit by the model will be crucial to achieving an increase in the precision of the primordial helium abundance determination.