Time Variation of Fine-Structure Constant Constrained by [O III] Emission-Lines at 1.1<z<3.7

Abstract

[O III]$λλ$4960,5008 doublet are often the strongest narrow emission lines in starburst galaxies and quasi-stellar objects (QSOs), and thus are a promising probe to possible variation of the fine-structure constant $α$ over cosmic time. Previous such studies using QSOs optical spectra were limited to $z<1$. In this work, we constructed a sample of 40 spectra of Ly$α$ emitting galaxies (LAEs) and a sample of 46 spectra of QSOs at $1.09<z<3.73$ using the VLT/X-Shooter near-infrared spectra publicly available. We measured the wavelength ratios of the two components of the spin-orbit doublet and accordingly calculated $α(z)$ using two methods. Analysis on all of the 86 spectra yielded $Δα/α=(-3\pm6)\times10^{-5}$ with respect to the laboratory $α$ measurements, consistent with no variation over the explored time interval. If assuming a uniform variation rate, we obtained $α^{-1}{\rm d}α/{\rm d}t = (-3\pm6)\times10^{-15}$ yr$^{-1}$ within the last 12 Gyrs. Extensive tests indicate that $α$ variation could be better constrained using starburst galaxies' spectra than using QSO spectra in future studies.