Primordial Lithium Abundance as a Stringent Constraint on the Baryonic   Content of the Universe
  We have refined the estimate of the primordial level of $^7$Li abundance to an accuracy better than 10%, based on high-precision Li abundances for metal-poor halo stars, and a recent model of post-BBN (Big Bang Nucleosynthesis) chemical evolution that provides a quantitative explanation of the detected gentle ascent of the Spite Plateau for stars with metallicities [Fe/H]$ > -3$. Our maximum likelihood analysis obtains an estimate for the primordial Li abundance of $A({\rm Li})_p=2.07^{+0.16}_{-0.04}$, after taking into account possible systematic errors in the estimation of Li abundances, with the exception of a still-controversial issue regarding stellar depletion. The inferred value of $\eta$ (the baryon-to-photon number-density ratio in the universe) based on this estimate is more consistent with that derived from the set of reported ``low He'' + ``high D'' from extragalactic sites than that derived from reported ``high He'' + ``low D'' measurements. Since, within current models of stellar depletion processes, it is difficult to account for the observed very small scatter of Li abundance in metal-poor stars, our estimate of $A({\rm Li})_p$ should be taken as an independent constraint on the baryonic mass density parameter in the universe, giving $\Omega_b h^2=(0.64-1.4)\times 10^{-2}$ with $h=H_0/100$ km s$^{-1}$Mpc$^{-1}$. 
Takeru Ken Suzuki, Yuzuru Yoshii, & Timothy C. Beers