The LBT $Y_{\rm p}$ Project I: An Improved Determination of the Primordial Helium Abundance -- Project Description, Sample Selection, Observations, and Methodology

TL;DR

This paper presents an improved method using LBT observations and new analysis techniques to measure the primordial helium abundance ($Y_{p}$) with high precision, aiming to constrain physics beyond the Standard Model.

Contribution

It introduces a novel analysis methodology combined with new LBT data to achieve more precise $Y_{p}$ measurements, reducing uncertainties to about 2%.

Findings

Achieved helium abundance uncertainties of approximately 2%.

Selected low-metallicity galaxy sample for precise $Y_{p}$ determination.

Projected $Y_{p}$ measurement precision of about 0.5%.

Abstract

Extremely low metallicity HII regions have been observed with the goal of determining the primordial helium abundance ($Y_{\rm p}$). $Y_{\rm p}$, combined with standard big bang nucleosynthesis and the half-life of the neutron, provides a direct measurement of the number of neutrino families, but $Y_{\rm p}$ must be measured very precisely to provide meaningful constraints on physics beyond the Standard Model. Here we describe a program to combine new Large Binocular Telescope (LBT) observations with a new analysis methodology to significantly improve the determination of $Y_{\rm p}$. The LBT, with its MODS and LUCI instruments, produces spectra, which, when combined with our new analysis methodology, are capable of delivering He abundances in individual HII regions with uncertainties of approximately 2% or less. Archival LBT/MODS spectra of standard stars over a four-year period enable the determination of a wavelength-dependent uncertainty in the MODS spectral response, resulting in improved relative emission line uncertainties. An optimized sample of low-metallicity galaxies has been selected with the goal of producing a determination of $Y_{\rm p}$ with a precision of $\sim$ 0.5%, sufficient to provide an independent constraint on the effective number of neutrino families of $\sim$ 3%.