Abundances of light elements in metal-poor stars III. Data analysis and results

We present the results of the analysis of an extensive set of new and liter ature high quality data concerning Fe, C, N, O, Na, and Mg. This analysis e xploited the T-eff scale determined in Gratton et al. (1996a), and the non- LTE abundance corrections computed in Gratton et al. (1999a). Results obtai ned with various abundance indices are discussed and compared. Derailed com parison with models of galactic chemical evolution will be presented in fut ure papers of this series. Our non-LTE analysis yields the same O abundances from both permitted and f orbidden lines for stars with T-eff >4600 K, in agree ment with King (1993) , but not with other studies using a lower T-eff -scale for subdwarfs. Howe ver, we obtain slightly smaller O abundances for the most luminous metal-po or field stars than for fainter stars of similar metallicities, an effect a ttributed to inadequacies of the adopted model atmospheres (Kurucz 1992, wi th overshooting) for cool stars. We find a nearly constant O overundance in metal-poor stars ([Fe/H]< -9.8), at a mean value of 0.46 +/- 0.02 dex(sigm a = 0.12, 32 stars), with only a gentle slope with [Fe/H] (similar to -0.1) ; this result is different from the steeper slope recently obtained using O H band in the near UV. If only bonafide unmixed stars are considered, C abundances scale with Fe o nes (i.e. [C/Fe]approximate to 0) down to [Fe/H]similar to -2.5. Due to our adoption of a different T-eff scale, we do not confirm the slight C excess in the most metal poor disk dwarfs (- 0.8 <[Fe/H]< -0.4) found in previous investigations. Na abundances scale as Fe ones in the high metallicity regime? while metal- poor stars present a Na underabundance. None of the field stars analyzed be long to the group of O-poor and Na-rich stars observed in globular clusters . Na is deficient with respect to ME in halo and thick disk stars; within t hese populations, Na deficiency may be a slow function of [Mg/H]. Salar [Na /Mg] ratios are obtained for thin disk stars.