We employ a new Infrared Flux Method ( IRFM ) temperature scale ( Ramírez & Meléndez 2005a , b ) 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 ( Meléndez & Ramírez 2004 ) is higher than previously reported values , but still lower than the primordial abundance suggested by WMAP data and BBN .