The advent of 8 m class telescopes has allowed the detailed spectroscopic study of sizeable numbers of extremely metal-poor Galactic stars which are the witnesses of the formation of the early Galaxy . Their chemical composition displays some distinctive trends which should provide a strong constraint on the physical nature of the first generation ( s ) of stars and on their nucleosynthetic output . I will review recent results in the field following the periodic table , from lithium to uranium and shortly comment on the intriguing classes of Carbon Enhanced Metal Poor ( CEMP ) stars , for many of which there is no analogue among solar metallicity stars . In spite of these exciting results , the number of known stars of metallicity below [ Fe/H ] =–3.3 remains quite small and it would be desirable to discover more , both to clearly understand the metal-weak tail of Halo metallicity distribution and to clarify the abundance trends at the lowest metallicities . Most of these extremely rare objects have been discovered by the wide field objective prism surveys , HK survey and Hamburg-ESO survey . In the near future the Sloan Digital Sky Survey and its continuation SEGUE are expected to boost significantly the numbers of known extremely metal poor stars . We are living exciting times but an even more exciting future lies ahead !