O and Fe abundance correlations and distributions inferred for the thick
  and thin disk
  A linear [Fe/H]-[O/H] relation is found for different stellar populations in
the Galaxy (halo, thick disk, thin disk) from a data sample obtained in a
recent investigation (Ram{\'\i}rez et al. 2013). These correlations support
previous 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 abundance
distributions are then determined for different subsamples, which are well
explained 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 gives
us clues about inflow/outflow rates in these different Galactic regions and
their corresponding evolution. Outflow rate for the thick and the thin disks
are lower than the halo outflow rate. Moreover if the thin disk built up from
the thick disk, both systems result of comparable masses. Besides that, the
iron-to-oxygen yield ratio and the primary to not primary contribution ratio
for the iron production are obtained from the data, resulting consistent with
SNII progenitor nucleosynthesis and with the iron production from SNIa
supernova events.
