The Temperature Scale of Metal-Poor Dwarfs: Lithium and Oxygen   Abundances
  We employ a new Infrared Flux Method (IRFM) temperature scale (Ramirez & Melendez 2005, ApJ 626, 446; ApJ 626, 465) in order to determine Li, O, and Fe NLTE abundances in a sample of relatively unevolved (dwarfs, turn-off, subgiants) metal-poor stars. We show that the analysis of the permitted OI triplet and FeII lines leads to a plateau in [OI/FeII] over the broad metallicity range -3.2 < [Fe/H] < -0.7, independent of temperature and metallicity, and with a star-to-star scatter of only 0.1 dex. The Li abundance in halo stars is also found to be independent of temperature and metallicity (Spite plateau), with a star-to-star scatter of just 0.06 dex over the metallicity range -3.4 < [Fe/H] < -1. Our Li abundance (Melendez & Ramirez 2004, ApJ 615, L33) is higher than previously reported values, but still lower than the primordial abundance suggested by WMAP data and BBN. 
Jorge Melendez, Nataliya G. Shchukina, Ivan Ramirez & Irina Vasiljeva