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A linear [Fe/H]-[O/H] relation is found for different stellar populations inthe Galaxy (halo, thick disk, thin disk) from a data sample obtained in arecent investigation (Ram{\'\i}rez et al. 2013). These correlations supportprevious results inferred from poorer samples: stars display a "main sequence"expressed as [Fe/H] = $a$[O/H$]+b\mp\Delta b$ where a unit slope, $a=1$,implies a constant [O/Fe] abundance ratio. Oxygen and iron empirical abundancedistributions are then determined for different subsamples, which are wellexplained by the theoretical predictions of multistage closed-(box+reservoir)(MCBR) chemical evolution models by taking into account the found correlations.The interpretation of these distributions in the framework of MCBR models givesus clues about inflow/outflow rates in these different Galactic regions andtheir corresponding evolution. Outflow rate for the thick and the thin disksare lower than the halo outflow rate. Moreover if the thin disk built up fromthe thick disk, both systems result of comparable masses. Besides that, theiron-to-oxygen yield ratio and the primary to not primary contribution ratiofor the iron production are obtained from the data, resulting consistent withSNII progenitor nucleosynthesis and with the iron production from SNIasupernova events.

O and Fe abundance correlations and distributions inferred for the thick and thin disk